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aria-controls="toc-Properties-sublist" class="cdx-button cdx-button--weight-quiet cdx-button--icon-only vector-toc-toggle"> <span class="vector-icon mw-ui-icon-wikimedia-expand"></span> <span>Toggle Properties subsection</span> </button> <ul id="toc-Properties-sublist" class="vector-toc-list"> <li id="toc-Equation_of_state" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Equation_of_state"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.1</span> <span>Equation of state</span> </div> </a> <ul id="toc-Equation_of_state-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Density_and_pressure" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Density_and_pressure"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.2</span> <span>Density and pressure</span> </div> </a> <ul id="toc-Density_and_pressure-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Current_constraints" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Current_constraints"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.3</span> <span>Current constraints</span> </div> </a> <ul id="toc-Current_constraints-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Tolman-Oppenheimer-Volkoff_Equation" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Tolman-Oppenheimer-Volkoff_Equation"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.4</span> <span>Tolman-Oppenheimer-Volkoff Equation</span> </div> </a> <ul id="toc-Tolman-Oppenheimer-Volkoff_Equation-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Mass-Radius_relation" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Mass-Radius_relation"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.5</span> <span>Mass-Radius relation</span> </div> </a> <ul id="toc-Mass-Radius_relation-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-I-Love-Q_Relations" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#I-Love-Q_Relations"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.6</span> <span>I-Love-Q Relations</span> </div> </a> <ul id="toc-I-Love-Q_Relations-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Temperature" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Temperature"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.7</span> <span>Temperature</span> </div> </a> <ul id="toc-Temperature-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Magnetic_field" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Magnetic_field"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.8</span> <span>Magnetic field</span> </div> </a> <ul id="toc-Magnetic_field-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Gravity" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Gravity"> <div class="vector-toc-text"> <span class="vector-toc-numb">2.9</span> <span>Gravity</span> </div> </a> <ul id="toc-Gravity-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Structure" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Structure"> <div class="vector-toc-text"> <span class="vector-toc-numb">3</span> <span>Structure</span> </div> </a> <ul id="toc-Structure-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Radiation" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Radiation"> <div class="vector-toc-text"> <span class="vector-toc-numb">4</span> <span>Radiation</span> </div> </a> <button aria-controls="toc-Radiation-sublist" class="cdx-button cdx-button--weight-quiet cdx-button--icon-only vector-toc-toggle"> <span class="vector-icon mw-ui-icon-wikimedia-expand"></span> <span>Toggle Radiation subsection</span> </button> <ul id="toc-Radiation-sublist" class="vector-toc-list"> <li id="toc-Pulsars" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Pulsars"> <div class="vector-toc-text"> <span class="vector-toc-numb">4.1</span> <span>Pulsars</span> </div> </a> <ul id="toc-Pulsars-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Non-pulsating_neutron_stars" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Non-pulsating_neutron_stars"> <div class="vector-toc-text"> <span class="vector-toc-numb">4.2</span> <span>Non-pulsating neutron stars</span> </div> </a> <ul id="toc-Non-pulsating_neutron_stars-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Spectra" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Spectra"> <div class="vector-toc-text"> <span class="vector-toc-numb">4.3</span> <span>Spectra</span> </div> </a> <ul id="toc-Spectra-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Rotation" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Rotation"> <div class="vector-toc-text"> <span class="vector-toc-numb">5</span> <span>Rotation</span> </div> </a> <button aria-controls="toc-Rotation-sublist" class="cdx-button cdx-button--weight-quiet cdx-button--icon-only vector-toc-toggle"> <span class="vector-icon mw-ui-icon-wikimedia-expand"></span> <span>Toggle Rotation subsection</span> </button> <ul id="toc-Rotation-sublist" class="vector-toc-list"> <li id="toc-Spin_down" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Spin_down"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.1</span> <span>Spin down</span> </div> </a> <ul id="toc-Spin_down-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Spin_up" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Spin_up"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.2</span> <span>Spin up</span> </div> </a> <ul id="toc-Spin_up-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Glitches_and_starquakes" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Glitches_and_starquakes"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.3</span> <span>Glitches and starquakes</span> </div> </a> <ul id="toc-Glitches_and_starquakes-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Anti-glitches" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Anti-glitches"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.4</span> <span>Anti-glitches</span> </div> </a> <ul id="toc-Anti-glitches-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Population_and_distances" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Population_and_distances"> <div class="vector-toc-text"> <span class="vector-toc-numb">6</span> <span>Population and distances</span> </div> </a> <ul id="toc-Population_and_distances-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Binary_neutron_star_systems" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Binary_neutron_star_systems"> <div class="vector-toc-text"> <span class="vector-toc-numb">7</span> <span>Binary neutron star systems</span> </div> </a> <button aria-controls="toc-Binary_neutron_star_systems-sublist" class="cdx-button cdx-button--weight-quiet cdx-button--icon-only vector-toc-toggle"> <span class="vector-icon mw-ui-icon-wikimedia-expand"></span> <span>Toggle Binary neutron star systems subsection</span> </button> <ul id="toc-Binary_neutron_star_systems-sublist" class="vector-toc-list"> <li id="toc-X-ray_binaries" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#X-ray_binaries"> <div class="vector-toc-text"> <span class="vector-toc-numb">7.1</span> <span>X-ray binaries</span> </div> </a> <ul id="toc-X-ray_binaries-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Neutron_star_binary_mergers_and_nucleosynthesis" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Neutron_star_binary_mergers_and_nucleosynthesis"> <div class="vector-toc-text"> <span class="vector-toc-numb">7.2</span> <span>Neutron star binary mergers and nucleosynthesis</span> </div> </a> <ul id="toc-Neutron_star_binary_mergers_and_nucleosynthesis-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Planets" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Planets"> <div class="vector-toc-text"> <span class="vector-toc-numb">8</span> <span>Planets</span> </div> </a> <ul id="toc-Planets-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-History_of_discoveries" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#History_of_discoveries"> <div class="vector-toc-text"> <span class="vector-toc-numb">9</span> <span>History of discoveries</span> </div> </a> <ul id="toc-History_of_discoveries-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Subtypes" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Subtypes"> <div class="vector-toc-text"> <span class="vector-toc-numb">10</span> <span>Subtypes</span> </div> </a> <ul id="toc-Subtypes-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Examples_of_neutron_stars" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Examples_of_neutron_stars"> <div class="vector-toc-text"> <span class="vector-toc-numb">11</span> <span>Examples of neutron stars</span> </div> </a> <ul id="toc-Examples_of_neutron_stars-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Gallery" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Gallery"> <div class="vector-toc-text"> <span class="vector-toc-numb">12</span> <span>Gallery</span> </div> </a> <ul id="toc-Gallery-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-See_also" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#See_also"> <div class="vector-toc-text"> <span class="vector-toc-numb">13</span> <span>See also</span> </div> </a> <ul id="toc-See_also-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Notes" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#Notes"> <div class="vector-toc-text"> <span class="vector-toc-numb">14</span> <span>Notes</span> </div> </a> <ul id="toc-Notes-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-References" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#References"> <div class="vector-toc-text"> <span class="vector-toc-numb">15</span> <span>References</span> </div> </a> <button aria-controls="toc-References-sublist" class="cdx-button cdx-button--weight-quiet cdx-button--icon-only vector-toc-toggle"> <span class="vector-icon mw-ui-icon-wikimedia-expand"></span> <span>Toggle References subsection</span> </button> <ul id="toc-References-sublist" class="vector-toc-list"> <li id="toc-Sources" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Sources"> <div class="vector-toc-text"> <span class="vector-toc-numb">15.1</span> <span>Sources</span> </div> </a> <ul id="toc-Sources-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-External_links" class="vector-toc-list-item vector-toc-level-1"> <a class="vector-toc-link" href="#External_links"> <div class="vector-toc-text"> <span class="vector-toc-numb">16</span> <span>External links</span> </div> </a> <ul id="toc-External_links-sublist" class="vector-toc-list"> </ul> </li> </ul> </div> </div> </nav> </div> </div> <div class="mw-content-container"> <main id="content" class="mw-body"> <header class="mw-body-header vector-page-titlebar"> <nav aria-label="Contents" class="vector-toc-landmark"> <div id="vector-page-titlebar-toc" class="vector-dropdown vector-page-titlebar-toc vector-button-flush-left" title="Table of Contents" > <input type="checkbox" id="vector-page-titlebar-toc-checkbox" role="button" aria-haspopup="true" data-event-name="ui.dropdown-vector-page-titlebar-toc" class="vector-dropdown-checkbox " aria-label="Toggle the table of contents" > <label id="vector-page-titlebar-toc-label" for="vector-page-titlebar-toc-checkbox" class="vector-dropdown-label cdx-button cdx-button--fake-button cdx-button--fake-button--enabled cdx-button--weight-quiet cdx-button--icon-only " aria-hidden="true" ><span class="vector-icon mw-ui-icon-listBullet mw-ui-icon-wikimedia-listBullet"></span> <span class="vector-dropdown-label-text">Toggle the table of contents</span> </label> <div class="vector-dropdown-content"> <div id="vector-page-titlebar-toc-unpinned-container" class="vector-unpinned-container"> </div> </div> </div> </nav> <h1 id="firstHeading" class="firstHeading mw-first-heading"><span class="mw-page-title-main">Neutron star</span></h1> <div id="p-lang-btn" class="vector-dropdown mw-portlet mw-portlet-lang" > <input type="checkbox" id="p-lang-btn-checkbox" role="button" aria-haspopup="true" data-event-name="ui.dropdown-p-lang-btn" class="vector-dropdown-checkbox mw-interlanguage-selector" aria-label="Go to an article in another language. Available in 88 languages" > <label id="p-lang-btn-label" for="p-lang-btn-checkbox" class="vector-dropdown-label cdx-button cdx-button--fake-button cdx-button--fake-button--enabled cdx-button--weight-quiet cdx-button--action-progressive mw-portlet-lang-heading-88" aria-hidden="true" ><span class="vector-icon mw-ui-icon-language-progressive mw-ui-icon-wikimedia-language-progressive"></span> <span class="vector-dropdown-label-text">88 languages</span> </label> <div class="vector-dropdown-content"> <div class="vector-menu-content"> <ul class="vector-menu-content-list"> <li class="interlanguage-link interwiki-af mw-list-item"><a href="https://af.wikipedia.org/wiki/Neutronster" title="Neutronster – Afrikaans" lang="af" hreflang="af" data-title="Neutronster" data-language-autonym="Afrikaans" data-language-local-name="Afrikaans" class="interlanguage-link-target"><span>Afrikaans</span></a></li><li class="interlanguage-link interwiki-anp mw-list-item"><a href="https://anp.wikipedia.org/wiki/%E0%A4%A8%E0%A5%8D%E0%A4%AF%E0%A5%82%E0%A4%9F%E0%A5%8D%E0%A4%B0%E0%A5%89%E0%A4%A8_%E0%A4%A4%E0%A4%BE%E0%A4%B0%E0%A4%BE" title="न्यूट्रॉन तारा – Angika" lang="anp" hreflang="anp" data-title="न्यूट्रॉन तारा" data-language-autonym="अंगिका" data-language-local-name="Angika" class="interlanguage-link-target"><span>अंगिका</span></a></li><li class="interlanguage-link interwiki-ar mw-list-item"><a href="https://ar.wikipedia.org/wiki/%D9%86%D8%AC%D9%85_%D9%86%D9%8A%D9%88%D8%AA%D8%B1%D9%88%D9%86%D9%8A" title="نجم نيوتروني – Arabic" lang="ar" hreflang="ar" data-title="نجم نيوتروني" data-language-autonym="العربية" data-language-local-name="Arabic" class="interlanguage-link-target"><span>العربية</span></a></li><li class="interlanguage-link interwiki-an mw-list-item"><a href="https://an.wikipedia.org/wiki/Estrela_de_neutrons" title="Estrela de neutrons – Aragonese" lang="an" hreflang="an" data-title="Estrela de neutrons" data-language-autonym="Aragonés" data-language-local-name="Aragonese" class="interlanguage-link-target"><span>Aragonés</span></a></li><li class="interlanguage-link interwiki-as mw-list-item"><a href="https://as.wikipedia.org/wiki/%E0%A6%A8%E0%A6%BF%E0%A6%89%E0%A6%9F%E0%A7%8D%E0%A7%B0%E0%A6%A8_%E0%A6%A4%E0%A7%B0%E0%A6%BE" title="নিউট্ৰন তৰা – Assamese" lang="as" hreflang="as" data-title="নিউট্ৰন তৰা" data-language-autonym="অসমীয়া" data-language-local-name="Assamese" class="interlanguage-link-target"><span>অসমীয়া</span></a></li><li class="interlanguage-link interwiki-ast mw-list-item"><a href="https://ast.wikipedia.org/wiki/Estrella_de_neutrones" title="Estrella de neutrones – Asturian" lang="ast" hreflang="ast" data-title="Estrella de neutrones" data-language-autonym="Asturianu" data-language-local-name="Asturian" class="interlanguage-link-target"><span>Asturianu</span></a></li><li class="interlanguage-link interwiki-az mw-list-item"><a href="https://az.wikipedia.org/wiki/Neytron_ulduzu" title="Neytron ulduzu – Azerbaijani" lang="az" hreflang="az" data-title="Neytron ulduzu" data-language-autonym="Azərbaycanca" data-language-local-name="Azerbaijani" class="interlanguage-link-target"><span>Azərbaycanca</span></a></li><li class="interlanguage-link interwiki-azb mw-list-item"><a href="https://azb.wikipedia.org/wiki/%D9%86%D9%88%D8%AA%D8%B1%D9%88%D9%86_%D8%A7%D9%88%D9%84%D8%AF%D9%88%D8%B2%D9%88" title="نوترون اولدوزو – South Azerbaijani" lang="azb" hreflang="azb" data-title="نوترون اولدوزو" data-language-autonym="تۆرکجه" data-language-local-name="South Azerbaijani" class="interlanguage-link-target"><span>تۆرکجه</span></a></li><li class="interlanguage-link interwiki-bn mw-list-item"><a href="https://bn.wikipedia.org/wiki/%E0%A6%A8%E0%A6%BF%E0%A6%89%E0%A6%9F%E0%A7%8D%E0%A6%B0%E0%A6%A8_%E0%A6%A4%E0%A6%BE%E0%A6%B0%E0%A6%BE" title="নিউট্রন তারা – Bangla" lang="bn" hreflang="bn" data-title="নিউট্রন তারা" data-language-autonym="বাংলা" data-language-local-name="Bangla" class="interlanguage-link-target"><span>বাংলা</span></a></li><li class="interlanguage-link interwiki-be mw-list-item"><a href="https://be.wikipedia.org/wiki/%D0%9D%D0%B5%D0%B9%D1%82%D1%80%D0%BE%D0%BD%D0%BD%D0%B0%D1%8F_%D0%B7%D0%BE%D1%80%D0%BA%D0%B0" title="Нейтронная зорка – Belarusian" lang="be" hreflang="be" data-title="Нейтронная зорка" data-language-autonym="Беларуская" data-language-local-name="Belarusian" class="interlanguage-link-target"><span>Беларуская</span></a></li><li class="interlanguage-link interwiki-be-x-old mw-list-item"><a href="https://be-tarask.wikipedia.org/wiki/%D0%9D%D1%8D%D1%9E%D1%82%D1%80%D0%BE%D0%BD%D0%BD%D0%B0%D1%8F_%D0%B7%D0%BE%D1%80%D0%BA%D0%B0" title="Нэўтронная зорка – Belarusian (Taraškievica orthography)" lang="be-tarask" hreflang="be-tarask" data-title="Нэўтронная зорка" data-language-autonym="Беларуская (тарашкевіца)" data-language-local-name="Belarusian (Taraškievica orthography)" class="interlanguage-link-target"><span>Беларуская (тарашкевіца)</span></a></li><li class="interlanguage-link interwiki-bg mw-list-item"><a href="https://bg.wikipedia.org/wiki/%D0%9D%D0%B5%D1%83%D1%82%D1%80%D0%BE%D0%BD%D0%BD%D0%B0_%D0%B7%D0%B2%D0%B5%D0%B7%D0%B4%D0%B0" title="Неутронна звезда – Bulgarian" lang="bg" hreflang="bg" data-title="Неутронна звезда" data-language-autonym="Български" data-language-local-name="Bulgarian" class="interlanguage-link-target"><span>Български</span></a></li><li class="interlanguage-link interwiki-bs mw-list-item"><a href="https://bs.wikipedia.org/wiki/Neutronska_zvijezda" title="Neutronska zvijezda – Bosnian" lang="bs" hreflang="bs" data-title="Neutronska zvijezda" data-language-autonym="Bosanski" data-language-local-name="Bosnian" class="interlanguage-link-target"><span>Bosanski</span></a></li><li class="interlanguage-link interwiki-ca mw-list-item"><a href="https://ca.wikipedia.org/wiki/Estrella_de_neutrons" title="Estrella de neutrons – Catalan" lang="ca" hreflang="ca" data-title="Estrella de neutrons" data-language-autonym="Català" data-language-local-name="Catalan" class="interlanguage-link-target"><span>Català</span></a></li><li class="interlanguage-link interwiki-cs mw-list-item"><a href="https://cs.wikipedia.org/wiki/Neutronov%C3%A1_hv%C4%9Bzda" title="Neutronová hvězda – Czech" lang="cs" hreflang="cs" data-title="Neutronová hvězda" data-language-autonym="Čeština" data-language-local-name="Czech" class="interlanguage-link-target"><span>Čeština</span></a></li><li class="interlanguage-link interwiki-cy mw-list-item"><a href="https://cy.wikipedia.org/wiki/Seren_niwtron" title="Seren niwtron – Welsh" lang="cy" hreflang="cy" data-title="Seren niwtron" data-language-autonym="Cymraeg" data-language-local-name="Welsh" class="interlanguage-link-target"><span>Cymraeg</span></a></li><li class="interlanguage-link interwiki-da mw-list-item"><a href="https://da.wikipedia.org/wiki/Neutronstjerne" title="Neutronstjerne – Danish" lang="da" hreflang="da" data-title="Neutronstjerne" data-language-autonym="Dansk" data-language-local-name="Danish" class="interlanguage-link-target"><span>Dansk</span></a></li><li class="interlanguage-link interwiki-de mw-list-item"><a href="https://de.wikipedia.org/wiki/Neutronenstern" title="Neutronenstern – German" lang="de" hreflang="de" data-title="Neutronenstern" data-language-autonym="Deutsch" data-language-local-name="German" class="interlanguage-link-target"><span>Deutsch</span></a></li><li class="interlanguage-link interwiki-et mw-list-item"><a href="https://et.wikipedia.org/wiki/Neutront%C3%A4ht" title="Neutrontäht – Estonian" lang="et" hreflang="et" data-title="Neutrontäht" data-language-autonym="Eesti" data-language-local-name="Estonian" class="interlanguage-link-target"><span>Eesti</span></a></li><li class="interlanguage-link interwiki-el mw-list-item"><a href="https://el.wikipedia.org/wiki/%CE%91%CF%83%CF%84%CE%AD%CF%81%CE%B1%CF%82_%CE%BD%CE%B5%CF%84%CF%81%CE%BF%CE%BD%CE%AF%CF%89%CE%BD" title="Αστέρας νετρονίων – Greek" lang="el" hreflang="el" data-title="Αστέρας νετρονίων" data-language-autonym="Ελληνικά" data-language-local-name="Greek" class="interlanguage-link-target"><span>Ελληνικά</span></a></li><li class="interlanguage-link interwiki-eml mw-list-item"><a href="https://eml.wikipedia.org/wiki/St%C3%A9la_%27d_neutr%C3%B2%E1%B9%85" title="Stéla 'd neutròṅ – Emiliano-Romagnolo" lang="egl" hreflang="egl" data-title="Stéla 'd neutròṅ" data-language-autonym="Emiliàn e rumagnòl" data-language-local-name="Emiliano-Romagnolo" class="interlanguage-link-target"><span>Emiliàn e rumagnòl</span></a></li><li class="interlanguage-link interwiki-es mw-list-item"><a href="https://es.wikipedia.org/wiki/Estrella_de_neutrones" title="Estrella de neutrones – Spanish" lang="es" hreflang="es" data-title="Estrella de neutrones" data-language-autonym="Español" data-language-local-name="Spanish" class="interlanguage-link-target"><span>Español</span></a></li><li class="interlanguage-link interwiki-eo mw-list-item"><a href="https://eo.wikipedia.org/wiki/Ne%C5%ADtrona_stelo" title="Neŭtrona stelo – Esperanto" lang="eo" hreflang="eo" data-title="Neŭtrona stelo" data-language-autonym="Esperanto" data-language-local-name="Esperanto" class="interlanguage-link-target"><span>Esperanto</span></a></li><li class="interlanguage-link interwiki-eu mw-list-item"><a href="https://eu.wikipedia.org/wiki/Neutroi-izar" title="Neutroi-izar – Basque" lang="eu" hreflang="eu" data-title="Neutroi-izar" data-language-autonym="Euskara" data-language-local-name="Basque" class="interlanguage-link-target"><span>Euskara</span></a></li><li class="interlanguage-link interwiki-fa mw-list-item"><a href="https://fa.wikipedia.org/wiki/%D8%B3%D8%AA%D8%A7%D8%B1%D9%87_%D9%86%D9%88%D8%AA%D8%B1%D9%88%D9%86%DB%8C" title="ستاره نوترونی – Persian" lang="fa" hreflang="fa" data-title="ستاره نوترونی" data-language-autonym="فارسی" data-language-local-name="Persian" class="interlanguage-link-target"><span>فارسی</span></a></li><li class="interlanguage-link interwiki-fr mw-list-item"><a href="https://fr.wikipedia.org/wiki/%C3%89toile_%C3%A0_neutrons" title="Étoile à neutrons – French" lang="fr" hreflang="fr" data-title="Étoile à neutrons" data-language-autonym="Français" data-language-local-name="French" class="interlanguage-link-target"><span>Français</span></a></li><li class="interlanguage-link interwiki-ga mw-list-item"><a href="https://ga.wikipedia.org/wiki/Neodr%C3%B3nr%C3%A9alta" title="Neodrónréalta – Irish" lang="ga" hreflang="ga" data-title="Neodrónréalta" data-language-autonym="Gaeilge" data-language-local-name="Irish" class="interlanguage-link-target"><span>Gaeilge</span></a></li><li class="interlanguage-link interwiki-gl mw-list-item"><a href="https://gl.wikipedia.org/wiki/Estrela_de_neutr%C3%B3ns" title="Estrela de neutróns – Galician" lang="gl" hreflang="gl" data-title="Estrela de neutróns" data-language-autonym="Galego" data-language-local-name="Galician" class="interlanguage-link-target"><span>Galego</span></a></li><li class="interlanguage-link interwiki-gu mw-list-item"><a href="https://gu.wikipedia.org/wiki/%E0%AA%A8%E0%AB%8D%E0%AA%AF%E0%AB%81%E0%AA%9F%E0%AB%8D%E0%AA%B0%E0%AB%8B%E0%AA%A8_%E0%AA%B8%E0%AB%8D%E0%AA%9F%E0%AA%BE%E0%AA%B0" title="ન્યુટ્રોન સ્ટાર – Gujarati" lang="gu" hreflang="gu" data-title="ન્યુટ્રોન સ્ટાર" data-language-autonym="ગુજરાતી" data-language-local-name="Gujarati" class="interlanguage-link-target"><span>ગુજરાતી</span></a></li><li class="interlanguage-link interwiki-ko mw-list-item"><a href="https://ko.wikipedia.org/wiki/%EC%A4%91%EC%84%B1%EC%9E%90%EB%B3%84" title="중성자별 – Korean" lang="ko" hreflang="ko" data-title="중성자별" data-language-autonym="한국어" data-language-local-name="Korean" class="interlanguage-link-target"><span>한국어</span></a></li><li class="interlanguage-link interwiki-hy mw-list-item"><a href="https://hy.wikipedia.org/wiki/%D5%86%D5%A5%D5%B5%D5%BF%D6%80%D5%B8%D5%B6%D5%A1%D5%B5%D5%AB%D5%B6_%D5%A1%D5%BD%D5%BF%D5%B2" title="Նեյտրոնային աստղ – Armenian" lang="hy" hreflang="hy" data-title="Նեյտրոնային աստղ" data-language-autonym="Հայերեն" data-language-local-name="Armenian" class="interlanguage-link-target"><span>Հայերեն</span></a></li><li class="interlanguage-link interwiki-hi mw-list-item"><a href="https://hi.wikipedia.org/wiki/%E0%A4%A8%E0%A5%8D%E0%A4%AF%E0%A5%82%E0%A4%9F%E0%A5%8D%E0%A4%B0%E0%A5%89%E0%A4%A8_%E0%A4%A4%E0%A4%BE%E0%A4%B0%E0%A4%BE" title="न्यूट्रॉन तारा – Hindi" lang="hi" hreflang="hi" data-title="न्यूट्रॉन तारा" data-language-autonym="हिन्दी" data-language-local-name="Hindi" class="interlanguage-link-target"><span>हिन्दी</span></a></li><li class="interlanguage-link interwiki-hr mw-list-item"><a href="https://hr.wikipedia.org/wiki/Neutronska_zvijezda" title="Neutronska zvijezda – Croatian" lang="hr" hreflang="hr" data-title="Neutronska zvijezda" data-language-autonym="Hrvatski" data-language-local-name="Croatian" class="interlanguage-link-target"><span>Hrvatski</span></a></li><li class="interlanguage-link interwiki-id mw-list-item"><a href="https://id.wikipedia.org/wiki/Bintang_neutron" title="Bintang neutron – Indonesian" lang="id" hreflang="id" data-title="Bintang neutron" data-language-autonym="Bahasa Indonesia" data-language-local-name="Indonesian" class="interlanguage-link-target"><span>Bahasa Indonesia</span></a></li><li class="interlanguage-link interwiki-is mw-list-item"><a href="https://is.wikipedia.org/wiki/Nifteindastj%C3%B6rnur" title="Nifteindastjörnur – Icelandic" lang="is" hreflang="is" data-title="Nifteindastjörnur" data-language-autonym="Íslenska" data-language-local-name="Icelandic" class="interlanguage-link-target"><span>Íslenska</span></a></li><li class="interlanguage-link interwiki-it mw-list-item"><a href="https://it.wikipedia.org/wiki/Stella_di_neutroni" title="Stella di neutroni – Italian" lang="it" hreflang="it" data-title="Stella di neutroni" data-language-autonym="Italiano" data-language-local-name="Italian" class="interlanguage-link-target"><span>Italiano</span></a></li><li class="interlanguage-link interwiki-he mw-list-item"><a href="https://he.wikipedia.org/wiki/%D7%9B%D7%95%D7%9B%D7%91_%D7%A0%D7%99%D7%99%D7%98%D7%A8%D7%95%D7%A0%D7%99%D7%9D" title="כוכב נייטרונים – Hebrew" lang="he" hreflang="he" data-title="כוכב נייטרונים" data-language-autonym="עברית" data-language-local-name="Hebrew" class="interlanguage-link-target"><span>עברית</span></a></li><li class="interlanguage-link interwiki-ka mw-list-item"><a href="https://ka.wikipedia.org/wiki/%E1%83%9C%E1%83%94%E1%83%98%E1%83%A2%E1%83%A0%E1%83%9D%E1%83%9C%E1%83%A3%E1%83%9A%E1%83%98_%E1%83%95%E1%83%90%E1%83%A0%E1%83%A1%E1%83%99%E1%83%95%E1%83%9A%E1%83%90%E1%83%95%E1%83%98" title="ნეიტრონული ვარსკვლავი – Georgian" lang="ka" hreflang="ka" data-title="ნეიტრონული ვარსკვლავი" data-language-autonym="ქართული" data-language-local-name="Georgian" class="interlanguage-link-target"><span>ქართული</span></a></li><li class="interlanguage-link interwiki-csb mw-list-item"><a href="https://csb.wikipedia.org/wiki/Ne%C3%B9tronow%C3%B4_gwi%C3%B4zda" title="Neùtronowô gwiôzda – Kashubian" lang="csb" hreflang="csb" data-title="Neùtronowô gwiôzda" data-language-autonym="Kaszëbsczi" data-language-local-name="Kashubian" class="interlanguage-link-target"><span>Kaszëbsczi</span></a></li><li class="interlanguage-link interwiki-kk mw-list-item"><a href="https://kk.wikipedia.org/wiki/%D0%9D%D0%B5%D0%B9%D1%82%D1%80%D0%BE%D0%BD_%D0%B6%D2%B1%D0%BB%D0%B4%D1%8B%D0%B7" title="Нейтрон жұлдыз – Kazakh" lang="kk" hreflang="kk" data-title="Нейтрон жұлдыз" data-language-autonym="Қазақша" data-language-local-name="Kazakh" class="interlanguage-link-target"><span>Қазақша</span></a></li><li class="interlanguage-link interwiki-ht mw-list-item"><a href="https://ht.wikipedia.org/wiki/Etwal_a_netwon" title="Etwal a netwon – Haitian Creole" lang="ht" hreflang="ht" data-title="Etwal a netwon" data-language-autonym="Kreyòl ayisyen" data-language-local-name="Haitian Creole" class="interlanguage-link-target"><span>Kreyòl ayisyen</span></a></li><li class="interlanguage-link interwiki-ky mw-list-item"><a href="https://ky.wikipedia.org/wiki/%D0%9D%D0%B5%D0%B9%D1%82%D1%80%D0%BE%D0%BD_%D0%B6%D1%8B%D0%BB%D0%B4%D1%8B%D0%B7%D1%8B" title="Нейтрон жылдызы – Kyrgyz" lang="ky" hreflang="ky" data-title="Нейтрон жылдызы" data-language-autonym="Кыргызча" data-language-local-name="Kyrgyz" class="interlanguage-link-target"><span>Кыргызча</span></a></li><li class="interlanguage-link interwiki-la mw-list-item"><a href="https://la.wikipedia.org/wiki/Stella_neutronica" title="Stella neutronica – Latin" lang="la" hreflang="la" data-title="Stella neutronica" data-language-autonym="Latina" data-language-local-name="Latin" class="interlanguage-link-target"><span>Latina</span></a></li><li class="interlanguage-link interwiki-lv mw-list-item"><a href="https://lv.wikipedia.org/wiki/Neitronu_zvaigzne" title="Neitronu zvaigzne – Latvian" lang="lv" hreflang="lv" data-title="Neitronu zvaigzne" data-language-autonym="Latviešu" data-language-local-name="Latvian" class="interlanguage-link-target"><span>Latviešu</span></a></li><li class="interlanguage-link interwiki-lt mw-list-item"><a href="https://lt.wikipedia.org/wiki/Neutronin%C4%97_%C5%BEvaig%C5%BEd%C4%97" title="Neutroninė žvaigždė – Lithuanian" lang="lt" hreflang="lt" data-title="Neutroninė žvaigždė" data-language-autonym="Lietuvių" data-language-local-name="Lithuanian" class="interlanguage-link-target"><span>Lietuvių</span></a></li><li class="interlanguage-link interwiki-hu mw-list-item"><a href="https://hu.wikipedia.org/wiki/Neutroncsillag" title="Neutroncsillag – Hungarian" lang="hu" hreflang="hu" data-title="Neutroncsillag" data-language-autonym="Magyar" data-language-local-name="Hungarian" class="interlanguage-link-target"><span>Magyar</span></a></li><li class="interlanguage-link interwiki-mk mw-list-item"><a href="https://mk.wikipedia.org/wiki/%D0%9D%D0%B5%D1%83%D1%82%D1%80%D0%BE%D0%BD%D1%81%D0%BA%D0%B0_%D1%95%D0%B2%D0%B5%D0%B7%D0%B4%D0%B0" title="Неутронска ѕвезда – Macedonian" lang="mk" hreflang="mk" data-title="Неутронска ѕвезда" data-language-autonym="Македонски" data-language-local-name="Macedonian" class="interlanguage-link-target"><span>Македонски</span></a></li><li class="interlanguage-link interwiki-ml mw-list-item"><a href="https://ml.wikipedia.org/wiki/%E0%B4%A8%E0%B5%8D%E0%B4%AF%E0%B5%82%E0%B4%9F%E0%B5%8D%E0%B4%B0%E0%B5%8B%E0%B5%BA_%E0%B4%A8%E0%B4%95%E0%B5%8D%E0%B4%B7%E0%B4%A4%E0%B5%8D%E0%B4%B0%E0%B4%82" title="ന്യൂട്രോൺ നക്ഷത്രം – Malayalam" lang="ml" hreflang="ml" data-title="ന്യൂട്രോൺ നക്ഷത്രം" data-language-autonym="മലയാളം" data-language-local-name="Malayalam" class="interlanguage-link-target"><span>മലയാളം</span></a></li><li class="interlanguage-link interwiki-mr mw-list-item"><a href="https://mr.wikipedia.org/wiki/%E0%A4%A8%E0%A5%8D%E0%A4%AF%E0%A5%82%E0%A4%9F%E0%A5%8D%E0%A4%B0%E0%A5%89%E0%A4%A8_%E0%A4%A4%E0%A4%BE%E0%A4%B0%E0%A4%BE" title="न्यूट्रॉन तारा – Marathi" lang="mr" hreflang="mr" data-title="न्यूट्रॉन तारा" data-language-autonym="मराठी" data-language-local-name="Marathi" class="interlanguage-link-target"><span>मराठी</span></a></li><li class="interlanguage-link interwiki-ms mw-list-item"><a href="https://ms.wikipedia.org/wiki/Bintang_neutron" title="Bintang neutron – Malay" lang="ms" hreflang="ms" data-title="Bintang neutron" data-language-autonym="Bahasa Melayu" data-language-local-name="Malay" class="interlanguage-link-target"><span>Bahasa Melayu</span></a></li><li class="interlanguage-link interwiki-min mw-list-item"><a href="https://min.wikipedia.org/wiki/Bintang_neutron" title="Bintang neutron – Minangkabau" lang="min" hreflang="min" data-title="Bintang neutron" data-language-autonym="Minangkabau" data-language-local-name="Minangkabau" class="interlanguage-link-target"><span>Minangkabau</span></a></li><li class="interlanguage-link interwiki-my mw-list-item"><a href="https://my.wikipedia.org/wiki/%E1%80%94%E1%80%9A%E1%80%B0%E1%80%91%E1%80%9B%E1%80%BD%E1%80%94%E1%80%BA%E1%80%80%E1%80%BC%E1%80%9A%E1%80%BA" title="နယူထရွန်ကြယ် – Burmese" lang="my" hreflang="my" data-title="နယူထရွန်ကြယ်" data-language-autonym="မြန်မာဘာသာ" data-language-local-name="Burmese" class="interlanguage-link-target"><span>မြန်မာဘာသာ</span></a></li><li class="interlanguage-link interwiki-fj mw-list-item"><a href="https://fj.wikipedia.org/wiki/Neutron_kalokalo" title="Neutron kalokalo – Fijian" lang="fj" hreflang="fj" data-title="Neutron kalokalo" data-language-autonym="Na Vosa Vakaviti" data-language-local-name="Fijian" class="interlanguage-link-target"><span>Na Vosa Vakaviti</span></a></li><li class="interlanguage-link interwiki-nl mw-list-item"><a href="https://nl.wikipedia.org/wiki/Neutronenster" title="Neutronenster – Dutch" lang="nl" hreflang="nl" data-title="Neutronenster" data-language-autonym="Nederlands" data-language-local-name="Dutch" class="interlanguage-link-target"><span>Nederlands</span></a></li><li class="interlanguage-link interwiki-ne mw-list-item"><a href="https://ne.wikipedia.org/wiki/%E0%A4%A8%E0%A5%8D%E0%A4%AF%E0%A5%81%E0%A4%9F%E0%A5%8D%E0%A4%B0%E0%A4%A8_%E0%A4%A4%E0%A4%BE%E0%A4%B0%E0%A4%BE" title="न्युट्रन तारा – Nepali" lang="ne" hreflang="ne" data-title="न्युट्रन तारा" data-language-autonym="नेपाली" data-language-local-name="Nepali" class="interlanguage-link-target"><span>नेपाली</span></a></li><li class="interlanguage-link interwiki-ja mw-list-item"><a href="https://ja.wikipedia.org/wiki/%E4%B8%AD%E6%80%A7%E5%AD%90%E6%98%9F" title="中性子星 – Japanese" lang="ja" hreflang="ja" data-title="中性子星" data-language-autonym="日本語" data-language-local-name="Japanese" class="interlanguage-link-target"><span>日本語</span></a></li><li class="interlanguage-link interwiki-no mw-list-item"><a href="https://no.wikipedia.org/wiki/N%C3%B8ytronstjerne" title="Nøytronstjerne – Norwegian Bokmål" lang="nb" hreflang="nb" data-title="Nøytronstjerne" data-language-autonym="Norsk bokmål" data-language-local-name="Norwegian Bokmål" class="interlanguage-link-target"><span>Norsk bokmål</span></a></li><li class="interlanguage-link interwiki-nn mw-list-item"><a href="https://nn.wikipedia.org/wiki/N%C3%B8ytronstjerne" title="Nøytronstjerne – Norwegian Nynorsk" lang="nn" hreflang="nn" data-title="Nøytronstjerne" data-language-autonym="Norsk nynorsk" data-language-local-name="Norwegian Nynorsk" class="interlanguage-link-target"><span>Norsk nynorsk</span></a></li><li class="interlanguage-link interwiki-oc mw-list-item"><a href="https://oc.wikipedia.org/wiki/Estela_de_neutrons" title="Estela de neutrons – Occitan" lang="oc" hreflang="oc" data-title="Estela de neutrons" data-language-autonym="Occitan" data-language-local-name="Occitan" class="interlanguage-link-target"><span>Occitan</span></a></li><li class="interlanguage-link interwiki-uz mw-list-item"><a href="https://uz.wikipedia.org/wiki/Neytron_yulduzlar" title="Neytron yulduzlar – Uzbek" lang="uz" hreflang="uz" data-title="Neytron yulduzlar" data-language-autonym="Oʻzbekcha / ўзбекча" data-language-local-name="Uzbek" class="interlanguage-link-target"><span>Oʻzbekcha / ўзбекча</span></a></li><li class="interlanguage-link interwiki-pa mw-list-item"><a href="https://pa.wikipedia.org/wiki/%E0%A8%A8%E0%A8%BF%E0%A8%89%E0%A8%9F%E0%A9%8D%E0%A8%B0%E0%A9%8B%E0%A8%A8_%E0%A8%A4%E0%A8%BE%E0%A8%B0%E0%A8%BE" title="ਨਿਉਟ੍ਰੋਨ ਤਾਰਾ – Punjabi" lang="pa" hreflang="pa" data-title="ਨਿਉਟ੍ਰੋਨ ਤਾਰਾ" data-language-autonym="ਪੰਜਾਬੀ" data-language-local-name="Punjabi" class="interlanguage-link-target"><span>ਪੰਜਾਬੀ</span></a></li><li class="interlanguage-link interwiki-pnb mw-list-item"><a href="https://pnb.wikipedia.org/wiki/%D9%86%DB%8C%D9%88%D9%B9%D8%B1%D9%88%D9%86_%D8%AA%D8%A7%D8%B1%DB%81" title="نیوٹرون تارہ – Western Punjabi" lang="pnb" hreflang="pnb" data-title="نیوٹرون تارہ" data-language-autonym="پنجابی" data-language-local-name="Western Punjabi" class="interlanguage-link-target"><span>پنجابی</span></a></li><li class="interlanguage-link interwiki-ps mw-list-item"><a href="https://ps.wikipedia.org/wiki/%D9%86%DB%8C%D9%88%D8%AA%D8%B1%D9%88%D9%86%D9%8A_%D8%B3%D8%AA%D9%88%D8%B1%DB%8C" title="نیوتروني ستوری – Pashto" lang="ps" hreflang="ps" data-title="نیوتروني ستوری" data-language-autonym="پښتو" data-language-local-name="Pashto" class="interlanguage-link-target"><span>پښتو</span></a></li><li class="interlanguage-link interwiki-pl mw-list-item"><a href="https://pl.wikipedia.org/wiki/Gwiazda_neutronowa" title="Gwiazda neutronowa – Polish" lang="pl" hreflang="pl" data-title="Gwiazda neutronowa" data-language-autonym="Polski" data-language-local-name="Polish" class="interlanguage-link-target"><span>Polski</span></a></li><li class="interlanguage-link interwiki-pt mw-list-item"><a href="https://pt.wikipedia.org/wiki/Estrela_de_n%C3%AAutrons" title="Estrela de nêutrons – Portuguese" lang="pt" hreflang="pt" data-title="Estrela de nêutrons" data-language-autonym="Português" data-language-local-name="Portuguese" class="interlanguage-link-target"><span>Português</span></a></li><li class="interlanguage-link interwiki-ro mw-list-item"><a href="https://ro.wikipedia.org/wiki/Stea_neutronic%C4%83" title="Stea neutronică – Romanian" lang="ro" hreflang="ro" data-title="Stea neutronică" data-language-autonym="Română" data-language-local-name="Romanian" class="interlanguage-link-target"><span>Română</span></a></li><li class="interlanguage-link interwiki-ru mw-list-item"><a href="https://ru.wikipedia.org/wiki/%D0%9D%D0%B5%D0%B9%D1%82%D1%80%D0%BE%D0%BD%D0%BD%D0%B0%D1%8F_%D0%B7%D0%B2%D0%B5%D0%B7%D0%B4%D0%B0" title="Нейтронная звезда – Russian" lang="ru" hreflang="ru" data-title="Нейтронная звезда" data-language-autonym="Русский" data-language-local-name="Russian" class="interlanguage-link-target"><span>Русский</span></a></li><li class="interlanguage-link interwiki-scn mw-list-item"><a href="https://scn.wikipedia.org/wiki/Stidda_di_niutroni" title="Stidda di niutroni – Sicilian" lang="scn" hreflang="scn" data-title="Stidda di niutroni" data-language-autonym="Sicilianu" data-language-local-name="Sicilian" class="interlanguage-link-target"><span>Sicilianu</span></a></li><li class="interlanguage-link interwiki-si mw-list-item"><a href="https://si.wikipedia.org/wiki/%E0%B6%B1%E0%B7%92%E0%B6%BA%E0%B7%94%E0%B6%A7%E0%B7%8A%E2%80%8D%E0%B6%BB%E0%B7%9D%E0%B6%B1_%E0%B6%AD%E0%B6%BB%E0%B7%94" title="නියුට්‍රෝන තරු – Sinhala" lang="si" hreflang="si" data-title="නියුට්‍රෝන තරු" data-language-autonym="සිංහල" data-language-local-name="Sinhala" class="interlanguage-link-target"><span>සිංහල</span></a></li><li class="interlanguage-link interwiki-simple mw-list-item"><a href="https://simple.wikipedia.org/wiki/Neutron_star" title="Neutron star – Simple English" lang="en-simple" hreflang="en-simple" data-title="Neutron star" data-language-autonym="Simple English" data-language-local-name="Simple English" class="interlanguage-link-target"><span>Simple English</span></a></li><li class="interlanguage-link interwiki-sk mw-list-item"><a href="https://sk.wikipedia.org/wiki/Neutr%C3%B3nov%C3%A1_hviezda" title="Neutrónová hviezda – Slovak" lang="sk" hreflang="sk" data-title="Neutrónová hviezda" data-language-autonym="Slovenčina" data-language-local-name="Slovak" class="interlanguage-link-target"><span>Slovenčina</span></a></li><li class="interlanguage-link interwiki-sl mw-list-item"><a href="https://sl.wikipedia.org/wiki/Nevtronska_zvezda" title="Nevtronska zvezda – Slovenian" lang="sl" hreflang="sl" data-title="Nevtronska zvezda" data-language-autonym="Slovenščina" data-language-local-name="Slovenian" class="interlanguage-link-target"><span>Slovenščina</span></a></li><li class="interlanguage-link interwiki-ckb mw-list-item"><a href="https://ckb.wikipedia.org/wiki/%D8%A6%DB%95%D8%B3%D8%AA%DB%8E%D8%B1%DB%95%DB%8C_%D9%86%DB%8C%D9%88%D8%AA%D8%B1%DB%86%D9%86%DB%8C" title="ئەستێرەی نیوترۆنی – Central Kurdish" lang="ckb" hreflang="ckb" data-title="ئەستێرەی نیوترۆنی" data-language-autonym="کوردی" data-language-local-name="Central Kurdish" class="interlanguage-link-target"><span>کوردی</span></a></li><li class="interlanguage-link interwiki-sr mw-list-item"><a href="https://sr.wikipedia.org/wiki/%D0%9D%D0%B5%D1%83%D1%82%D1%80%D0%BE%D0%BD%D1%81%D0%BA%D0%B0_%D0%B7%D0%B2%D0%B5%D0%B7%D0%B4%D0%B0" title="Неутронска звезда – Serbian" lang="sr" hreflang="sr" data-title="Неутронска звезда" data-language-autonym="Српски / srpski" data-language-local-name="Serbian" class="interlanguage-link-target"><span>Српски / srpski</span></a></li><li class="interlanguage-link interwiki-sh mw-list-item"><a href="https://sh.wikipedia.org/wiki/Neutronska_zvijezda" title="Neutronska zvijezda – Serbo-Croatian" lang="sh" hreflang="sh" data-title="Neutronska zvijezda" data-language-autonym="Srpskohrvatski / српскохрватски" data-language-local-name="Serbo-Croatian" class="interlanguage-link-target"><span>Srpskohrvatski / српскохрватски</span></a></li><li class="interlanguage-link interwiki-fi mw-list-item"><a href="https://fi.wikipedia.org/wiki/Neutronit%C3%A4hti" title="Neutronitähti – Finnish" lang="fi" hreflang="fi" data-title="Neutronitähti" data-language-autonym="Suomi" data-language-local-name="Finnish" class="interlanguage-link-target"><span>Suomi</span></a></li><li class="interlanguage-link interwiki-sv mw-list-item"><a href="https://sv.wikipedia.org/wiki/Neutronstj%C3%A4rna" title="Neutronstjärna – Swedish" lang="sv" hreflang="sv" data-title="Neutronstjärna" data-language-autonym="Svenska" data-language-local-name="Swedish" class="interlanguage-link-target"><span>Svenska</span></a></li><li class="interlanguage-link interwiki-ta mw-list-item"><a href="https://ta.wikipedia.org/wiki/%E0%AE%A8%E0%AF%8A%E0%AE%A4%E0%AF%81%E0%AE%AE%E0%AE%BF_%E0%AE%B5%E0%AE%BF%E0%AE%A3%E0%AF%8D%E0%AE%AE%E0%AF%80%E0%AE%A9%E0%AF%8D" title="நொதுமி விண்மீன் – Tamil" lang="ta" hreflang="ta" data-title="நொதுமி விண்மீன்" data-language-autonym="தமிழ்" data-language-local-name="Tamil" class="interlanguage-link-target"><span>தமிழ்</span></a></li><li class="interlanguage-link interwiki-tt mw-list-item"><a href="https://tt.wikipedia.org/wiki/%D0%9D%D0%B5%D0%B9%D1%82%D1%80%D0%BE%D0%BD_%D0%B9%D0%BE%D0%BB%D0%B4%D1%8B%D0%B7" title="Нейтрон йолдыз – Tatar" lang="tt" hreflang="tt" data-title="Нейтрон йолдыз" data-language-autonym="Татарча / tatarça" data-language-local-name="Tatar" class="interlanguage-link-target"><span>Татарча / tatarça</span></a></li><li class="interlanguage-link interwiki-te mw-list-item"><a href="https://te.wikipedia.org/wiki/%E0%B0%A8%E0%B1%8D%E0%B0%AF%E0%B1%82%E0%B0%9F%E0%B1%8D%E0%B0%B0%E0%B0%BE%E0%B0%A8%E0%B1%8D_%E0%B0%A4%E0%B0%BE%E0%B0%B0" title="న్యూట్రాన్ తార – Telugu" lang="te" hreflang="te" data-title="న్యూట్రాన్ తార" data-language-autonym="తెలుగు" data-language-local-name="Telugu" class="interlanguage-link-target"><span>తెలుగు</span></a></li><li class="interlanguage-link interwiki-th mw-list-item"><a href="https://th.wikipedia.org/wiki/%E0%B8%94%E0%B8%B2%E0%B8%A7%E0%B8%99%E0%B8%B4%E0%B8%A7%E0%B8%95%E0%B8%A3%E0%B8%AD%E0%B8%99" title="ดาวนิวตรอน – Thai" lang="th" hreflang="th" data-title="ดาวนิวตรอน" data-language-autonym="ไทย" data-language-local-name="Thai" class="interlanguage-link-target"><span>ไทย</span></a></li><li class="interlanguage-link interwiki-tr mw-list-item"><a href="https://tr.wikipedia.org/wiki/N%C3%B6tron_y%C4%B1ld%C4%B1z%C4%B1" title="Nötron yıldızı – Turkish" lang="tr" hreflang="tr" data-title="Nötron yıldızı" data-language-autonym="Türkçe" data-language-local-name="Turkish" class="interlanguage-link-target"><span>Türkçe</span></a></li><li class="interlanguage-link interwiki-uk mw-list-item"><a href="https://uk.wikipedia.org/wiki/%D0%9D%D0%B5%D0%B9%D1%82%D1%80%D0%BE%D0%BD%D0%BD%D0%B0_%D0%B7%D0%BE%D1%80%D1%8F" title="Нейтронна зоря – Ukrainian" lang="uk" hreflang="uk" data-title="Нейтронна зоря" data-language-autonym="Українська" data-language-local-name="Ukrainian" class="interlanguage-link-target"><span>Українська</span></a></li><li class="interlanguage-link interwiki-vi mw-list-item"><a href="https://vi.wikipedia.org/wiki/Sao_neutron" title="Sao neutron – Vietnamese" lang="vi" hreflang="vi" data-title="Sao neutron" data-language-autonym="Tiếng Việt" data-language-local-name="Vietnamese" class="interlanguage-link-target"><span>Tiếng Việt</span></a></li><li class="interlanguage-link interwiki-zh-classical mw-list-item"><a href="https://zh-classical.wikipedia.org/wiki/%E4%B8%AD%E5%AD%90%E6%98%9F" title="中子星 – Literary Chinese" lang="lzh" hreflang="lzh" data-title="中子星" data-language-autonym="文言" data-language-local-name="Literary Chinese" class="interlanguage-link-target"><span>文言</span></a></li><li class="interlanguage-link interwiki-wuu mw-list-item"><a href="https://wuu.wikipedia.org/wiki/%E4%B8%AD%E5%AD%90%E6%98%9F" title="中子星 – Wu" lang="wuu" hreflang="wuu" data-title="中子星" data-language-autonym="吴语" data-language-local-name="Wu" class="interlanguage-link-target"><span>吴语</span></a></li><li class="interlanguage-link interwiki-zh-yue mw-list-item"><a href="https://zh-yue.wikipedia.org/wiki/%E4%B8%AD%E5%AD%90%E6%98%9F" title="中子星 – Cantonese" lang="yue" hreflang="yue" data-title="中子星" data-language-autonym="粵語" data-language-local-name="Cantonese" class="interlanguage-link-target"><span>粵語</span></a></li><li class="interlanguage-link interwiki-zh mw-list-item"><a href="https://zh.wikipedia.org/wiki/%E4%B8%AD%E5%AD%90%E6%98%9F" title="中子星 – Chinese" lang="zh" hreflang="zh" data-title="中子星" 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class="mw-content-ltr mw-parser-output" lang="en" dir="ltr"><div class="shortdescription nomobile noexcerpt noprint searchaux" style="display:none">Collapsed core of a massive star</div> <style data-mw-deduplicate="TemplateStyles:r1236090951">.mw-parser-output .hatnote{font-style:italic}.mw-parser-output div.hatnote{padding-left:1.6em;margin-bottom:0.5em}.mw-parser-output .hatnote i{font-style:normal}.mw-parser-output .hatnote+link+.hatnote{margin-top:-0.5em}@media print{body.ns-0 .mw-parser-output .hatnote{display:none!important}}</style><div role="note" class="hatnote navigation-not-searchable">For other uses, see <a href="/wiki/Neutron_Star_(disambiguation)" class="mw-disambig" title="Neutron Star (disambiguation)">Neutron Star</a>.</div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Moving_heart_of_the_Crab_Nebula.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/8/8c/Moving_heart_of_the_Crab_Nebula.jpg/310px-Moving_heart_of_the_Crab_Nebula.jpg" decoding="async" width="310" height="303" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/8/8c/Moving_heart_of_the_Crab_Nebula.jpg/465px-Moving_heart_of_the_Crab_Nebula.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/8/8c/Moving_heart_of_the_Crab_Nebula.jpg/620px-Moving_heart_of_the_Crab_Nebula.jpg 2x" data-file-width="2125" data-file-height="2077" /></a><figcaption>Central neutron star at the heart of the <a href="/wiki/Crab_Nebula" title="Crab Nebula">Crab Nebula</a></figcaption></figure> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:PIA18848-PSRB1509-58-ChandraXRay-WiseIR-20141023.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/a/a6/PIA18848-PSRB1509-58-ChandraXRay-WiseIR-20141023.jpg/310px-PIA18848-PSRB1509-58-ChandraXRay-WiseIR-20141023.jpg" decoding="async" width="310" height="310" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/a/a6/PIA18848-PSRB1509-58-ChandraXRay-WiseIR-20141023.jpg/465px-PIA18848-PSRB1509-58-ChandraXRay-WiseIR-20141023.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/a/a6/PIA18848-PSRB1509-58-ChandraXRay-WiseIR-20141023.jpg/620px-PIA18848-PSRB1509-58-ChandraXRay-WiseIR-20141023.jpg 2x" data-file-width="3600" data-file-height="3600" /></a><figcaption>Radiation from the rapidly spinning <a href="/wiki/Pulsar" title="Pulsar">pulsar</a> <a href="/wiki/PSR_B1509-58" class="mw-redirect" title="PSR B1509-58">PSR B1509-58</a> makes nearby gas emit <a href="/wiki/X-ray" title="X-ray">X-rays</a> (gold) and illuminates the rest of the <a href="/wiki/Nebula" title="Nebula">nebula</a>, here seen in <a href="/wiki/Infrared" title="Infrared">infrared</a> (blue and red).</figcaption></figure> <p>A <b>neutron star</b> is the <a href="/wiki/Gravitational_collapse" title="Gravitational collapse">collapsed</a> <a href="/wiki/Stellar_structure" title="Stellar structure">core</a> of a massive <a href="/wiki/Supergiant_star" class="mw-redirect" title="Supergiant star">supergiant star</a>. It results from the <a href="/wiki/Supernova" title="Supernova">supernova</a> explosion of a <a href="/wiki/Stellar_evolution#Massive_star" title="Stellar evolution">massive star</a>—combined with <a href="/wiki/Gravitational_collapse" title="Gravitational collapse">gravitational collapse</a>—that compresses the core past <a href="/wiki/White_dwarf" title="White dwarf">white dwarf</a> star density to that of <a href="/wiki/Atomic_nucleus" title="Atomic nucleus">atomic nuclei</a>. Surpassed only by <a href="/wiki/Black_hole" title="Black hole">black holes</a>, neutron stars are the second smallest and densest known class of stellar objects.<sup id="cite_ref-1" class="reference"><a href="#cite_note-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup> Neutron stars have a radius on the order of 10 kilometers (6 mi) and a mass of about 1.4 <var>M</var><sub>☉</sub>.<sup id="cite_ref-2" class="reference"><a href="#cite_note-2"><span class="cite-bracket">[</span>2<span class="cite-bracket">]</span></a></sup> Stars that collapse into neutron stars have a total <a href="/wiki/Mass" title="Mass">mass</a> of between 10 and 25 <a href="/wiki/Solar_mass" title="Solar mass">solar masses</a> (<var>M</var><sub>☉</sub>), or possibly more for those that are especially rich in <a href="/wiki/Metallicity" title="Metallicity">elements heavier than hydrogen and helium</a>.<sup id="cite_ref-3" class="reference"><a href="#cite_note-3"><span class="cite-bracket">[</span>3<span class="cite-bracket">]</span></a></sup> </p><p>Once formed, neutron stars no longer actively generate heat and cool over time, but they may still evolve further through <a href="/wiki/Stellar_collision" title="Stellar collision">collisions</a> or <a href="/wiki/Accretion_(astrophysics)" title="Accretion (astrophysics)">accretion</a>. Most of the basic models for these objects imply that they are composed almost entirely of <a href="/wiki/Neutron" title="Neutron">neutrons</a>, as the extreme pressure causes the <a href="/wiki/Electron" title="Electron">electrons</a> and <a href="/wiki/Proton" title="Proton">protons</a> present in normal matter to combine into additional neutrons. These stars are partially supported against further collapse by <a href="/wiki/Degenerate_matter#Neutron_degeneracy" title="Degenerate matter">neutron degeneracy pressure</a>, just as <a href="/wiki/White_dwarf" title="White dwarf">white dwarfs</a> are supported against collapse by <a href="/wiki/Electron_degeneracy_pressure" title="Electron degeneracy pressure">electron degeneracy pressure</a>. However, this is not by itself sufficient to hold up an object beyond 0.7 <a href="/wiki/Solar_mass" title="Solar mass"><var>M</var><sub>☉</sub></a><sup id="cite_ref-4" class="reference"><a href="#cite_note-4"><span class="cite-bracket">[</span>4<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-5" class="reference"><a href="#cite_note-5"><span class="cite-bracket">[</span>5<span class="cite-bracket">]</span></a></sup> and repulsive nuclear forces increasingly contribute to supporting more massive neutron stars.<sup id="cite_ref-6" class="reference"><a href="#cite_note-6"><span class="cite-bracket">[</span>6<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-7" class="reference"><a href="#cite_note-7"><span class="cite-bracket">[</span>7<span class="cite-bracket">]</span></a></sup> If the remnant star has a <a href="/wiki/Mass" title="Mass">mass</a> exceeding the <a href="/wiki/Tolman%E2%80%93Oppenheimer%E2%80%93Volkoff_limit" title="Tolman–Oppenheimer–Volkoff limit">Tolman–Oppenheimer–Volkoff limit</a>, which ranges from <span class="nowrap">2.2–2.9 <var>M</var><sub>☉</sub>,</span> the combination of degeneracy pressure and nuclear forces is insufficient to support the neutron star, causing it to collapse and form a <a href="/wiki/Black_hole" title="Black hole">black hole</a>. The most massive neutron star detected so far, <a href="/wiki/PSR_J0952%E2%80%930607" title="PSR J0952–0607">PSR J0952–0607</a>, is estimated to be <span class="nowrap"><span data-sort-value="7030467309250000000♠"></span>2.35<span style="margin-left:0.3em;margin-right:0.15em;">±</span>0.17 <i>M</i><sub>☉</sub></span>.<sup id="cite_ref-blackwidow_8-0" class="reference"><a href="#cite_note-blackwidow-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup> </p><p>Newly formed neutron stars may have surface temperatures of ten million K or more. However, since neutron stars generate no new heat through fusion, they inexorably cool down after their formation. Consequently, a given neutron star reaches a surface temperature of one million K when it is between one thousand and one million years old.<sup id="cite_ref-Chandra_9-0" class="reference"><a href="#cite_note-Chandra-9"><span class="cite-bracket">[</span>9<span class="cite-bracket">]</span></a></sup> Older and even-cooler neutron stars are still easy to discover. For example, the well-studied neutron star, <span class="nowrap"><a href="/wiki/RX_J1856.5%E2%88%923754" title="RX J1856.5−3754">RX J1856.5−3754</a>,</span> has an average surface temperature of about 434,000 K.<sup id="cite_ref-10" class="reference"><a href="#cite_note-10"><span class="cite-bracket">[</span>10<span class="cite-bracket">]</span></a></sup> For comparison, the Sun has an effective surface temperature of 5,780 K.<sup id="cite_ref-11" class="reference"><a href="#cite_note-11"><span class="cite-bracket">[</span>11<span class="cite-bracket">]</span></a></sup> </p><p>Neutron star material is remarkably <a href="/wiki/Density" title="Density">dense</a>: a normal-sized <a href="/wiki/Phillumeny#Matchbox" title="Phillumeny">matchbox</a> containing neutron-star material would have a weight of approximately 3 <a href="/wiki/Billion" title="Billion">billion</a> tonnes, the same weight as a 0.5-cubic-kilometer chunk of the Earth (a cube with edges of about 800 meters) from Earth's surface.<sup id="cite_ref-12" class="reference"><a href="#cite_note-12"><span class="cite-bracket">[</span>12<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-13" class="reference"><a href="#cite_note-13"><span class="cite-bracket">[</span>13<span class="cite-bracket">]</span></a></sup> </p><p>As a star's core collapses, its rotation rate increases due to <a href="/wiki/Conservation_of_angular_momentum" class="mw-redirect" title="Conservation of angular momentum">conservation of angular momentum</a>, so newly formed neutron stars typically rotate at up to several hundred times per second. Some neutron stars emit beams of electromagnetic radiation that make them detectable as pulsars, and the discovery of pulsars by <a href="/wiki/Jocelyn_Bell_Burnell" title="Jocelyn Bell Burnell">Jocelyn Bell Burnell</a> and <a href="/wiki/Antony_Hewish" title="Antony Hewish">Antony Hewish</a> in 1967 was the first observational suggestion that neutron stars exist. The fastest-spinning neutron star known is <a href="/wiki/PSR_J1748%E2%88%922446ad" title="PSR J1748−2446ad">PSR J1748−2446ad</a>, rotating at a rate of 716 times per second<sup id="cite_ref-14" class="reference"><a href="#cite_note-14"><span class="cite-bracket">[</span>14<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-15" class="reference"><a href="#cite_note-15"><span class="cite-bracket">[</span>15<span class="cite-bracket">]</span></a></sup> or 43,000 <a href="/wiki/Revolutions_per_minute" title="Revolutions per minute">revolutions per minute</a>, giving a linear (tangential) speed at the surface on the order of 0.24<i>c</i> (i.e., nearly a quarter the <a href="/wiki/Speed_of_light" title="Speed of light">speed of light</a>). </p><p>There are thought to be around one billion neutron stars in the <a href="/wiki/Milky_Way" title="Milky Way">Milky Way</a>,<sup id="cite_ref-16" class="reference"><a href="#cite_note-16"><span class="cite-bracket">[</span>16<span class="cite-bracket">]</span></a></sup> and at a minimum several hundred million, a figure obtained by estimating the number of stars that have undergone supernova explosions.<sup id="cite_ref-17" class="reference"><a href="#cite_note-17"><span class="cite-bracket">[</span>17<span class="cite-bracket">]</span></a></sup> However, many of them have existed for a long period of time and have cooled down considerably. These stars radiate very little electromagnetic radiation; most neutron stars that have been detected occur only in certain situations in which they do radiate, such as if they are a pulsar or a part of a binary system. Slow-rotating and non-accreting neutron stars are difficult to detect, due to the absence of electromagnetic radiation; however, since the <a href="/wiki/Hubble_Space_Telescope" title="Hubble Space Telescope">Hubble Space Telescope</a>'s detection of <a href="/wiki/RX_J1856.5%E2%88%923754" title="RX J1856.5−3754">RX J1856.5−3754</a> in the 1990s, a few nearby neutron stars that appear to emit only thermal radiation have been detected. </p><p>Neutron stars in binary systems can undergo accretion, in which case they emit large amounts of <a href="/wiki/X-ray" title="X-ray">X-rays</a>. During this process, matter is deposited on the surface of the stars, forming "hotspots" that can be sporadically identified as <a href="/wiki/X-ray_pulsar" title="X-ray pulsar">X-ray pulsar</a> systems. Additionally, such accretions are able to "recycle" old pulsars, causing them to gain mass and rotate extremely quickly, forming <a href="/wiki/Millisecond_pulsar" title="Millisecond pulsar">millisecond pulsars</a>. Furthermore, binary systems such as these continue to <a href="/wiki/Stellar_evolution" title="Stellar evolution">evolve</a>, with many companions eventually becoming <a href="/wiki/Compact_star" class="mw-redirect" title="Compact star">compact objects</a> such as white dwarfs or neutron stars themselves, though other possibilities include a complete destruction of the companion through <a href="/wiki/Ablation" title="Ablation">ablation</a> or collision. </p><p>The study of neutron star systems is central to <a href="/wiki/Gravitational_wave" title="Gravitational wave">gravitational wave</a> astronomy. The <a href="/wiki/Neutron_star_merger" title="Neutron star merger">merger of binary neutron stars</a> produces gravitational waves and may be associated with <a href="/wiki/Kilonova" title="Kilonova">kilonovae</a> and <a href="/wiki/Gamma-ray_burst" title="Gamma-ray burst">short-duration gamma-ray bursts</a>. In 2017, the <a href="/wiki/LIGO" title="LIGO">LIGO</a> and <a href="/wiki/Virgo_interferometer" title="Virgo interferometer">Virgo</a> interferometer sites observed <a href="/wiki/GW170817" title="GW170817">GW170817</a>, the first direct detection of gravitational waves from such an event.<sup id="cite_ref-18" class="reference"><a href="#cite_note-18"><span class="cite-bracket">[</span>18<span class="cite-bracket">]</span></a></sup> Prior to this, indirect evidence for gravitational waves was inferred by studying the gravity radiated from the orbital decay of a different type of (unmerged) binary neutron system, the <a href="/wiki/Hulse%E2%80%93Taylor_pulsar" title="Hulse–Taylor pulsar">Hulse–Taylor pulsar</a>. </p> <meta property="mw:PageProp/toc" /> <div class="mw-heading mw-heading2"><h2 id="Formation">Formation</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=1" title="Edit section: Formation"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Neutronstarsimple.png" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/c/c7/Neutronstarsimple.png/220px-Neutronstarsimple.png" decoding="async" width="220" height="220" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/c/c7/Neutronstarsimple.png/330px-Neutronstarsimple.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/c/c7/Neutronstarsimple.png/440px-Neutronstarsimple.png 2x" data-file-width="14000" data-file-height="14000" /></a><figcaption>Simplified representation of the formation of neutron stars</figcaption></figure> <p>Any <a href="/wiki/Main_sequence" title="Main sequence">main-sequence</a> star with an initial mass of greater than 8 <a href="/wiki/Solar_mass" title="Solar mass"><var>M</var><sub>☉</sub></a> (eight times the mass of the <a href="/wiki/Sun" title="Sun">Sun</a>) has the potential to become a neutron star. As the star evolves away from the main sequence, <a href="/wiki/Stellar_nucleosynthesis" title="Stellar nucleosynthesis">stellar nucleosynthesis</a> produces an iron-rich core. When all nuclear fuel in the core has been exhausted, the core must be supported by degeneracy pressure alone. Further deposits of mass from shell burning cause the core to exceed the <a href="/wiki/Chandrasekhar_limit" title="Chandrasekhar limit">Chandrasekhar limit</a>. Electron-degeneracy pressure is overcome, and the core collapses further, causing temperatures to rise to over <span class="nowrap"><span data-sort-value="7009500000000000000♠"></span>5<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>9</sup> K</span> (5 billion K). At these temperatures, <a href="/wiki/Photodisintegration" title="Photodisintegration">photodisintegration</a> (the breakdown of iron nuclei into <a href="/wiki/Alpha_particle" title="Alpha particle">alpha particles</a> due to high-energy gamma rays) occurs. As the temperature of the core continues to rise, electrons and protons combine to form neutrons via <a href="/wiki/Electron_capture" title="Electron capture">electron capture</a>, releasing a flood of <a href="/wiki/Neutrino" title="Neutrino">neutrinos</a>. When densities reach a nuclear density of <span class="nowrap"><span data-sort-value="7017400000000000000♠"></span>4<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>17</sup> kg/m<sup>3</sup></span>, a combination of <a href="/wiki/Strong_force" class="mw-redirect" title="Strong force">strong force</a> repulsion and neutron degeneracy pressure halts the contraction.<sup id="cite_ref-19" class="reference"><a href="#cite_note-19"><span class="cite-bracket">[</span>19<span class="cite-bracket">]</span></a></sup> The contracting outer envelope of the star is halted and rapidly flung outwards by a flux of neutrinos produced in the creation of the neutrons, resulting in a <a href="/wiki/Supernova" title="Supernova">supernova</a> and leaving behind a neutron star. However, if the remnant has a mass greater than about 3 <var>M</var><sub>☉</sub>, it instead becomes a black hole.<sup id="cite_ref-20" class="reference"><a href="#cite_note-20"><span class="cite-bracket">[</span>20<span class="cite-bracket">]</span></a></sup> </p><p>As the core of a massive star is compressed during a <a href="/wiki/Type_II_supernova" title="Type II supernova">Type II supernova</a> or a <a href="/wiki/Type_Ib_and_Ic_supernovae" title="Type Ib and Ic supernovae">Type Ib or Type Ic</a> supernova, and collapses into a neutron star, it retains most of its <a href="/wiki/Angular_momentum" title="Angular momentum">angular momentum</a>. Because it has only a tiny fraction of its parent's radius (sharply reducing its <a href="/wiki/Moment_of_inertia" title="Moment of inertia">moment of inertia</a>), a neutron star is formed with very high rotation speed and then, over a very long period, it slows. Neutron stars are known that have rotation periods from about 1.4 ms to 30 s. The neutron star's density also gives it very high <a href="/wiki/Surface_gravity" title="Surface gravity">surface gravity</a>, with typical values ranging from <span class="nowrap"><span data-sort-value="7012100000000000000♠"></span>10<sup>12</sup></span> to <span class="nowrap"><span data-sort-value="7013100000000000000♠"></span>10<sup>13</sup> m/s<sup>2</sup></span> (more than <span class="nowrap"><span data-sort-value="7011100000000000000♠"></span>10<sup>11</sup></span> times that of <a href="/wiki/Earth" title="Earth">Earth</a>).<sup id="cite_ref-Haensel_21-0" class="reference"><a href="#cite_note-Haensel-21"><span class="cite-bracket">[</span>21<span class="cite-bracket">]</span></a></sup> One measure of such immense gravity is the fact that neutron stars have an <a href="/wiki/Escape_velocity" title="Escape velocity">escape velocity</a> of over half the <a href="/wiki/Speed_of_light" title="Speed of light">speed of light</a>.<sup id="cite_ref-ChandraBlog_2013_22-0" class="reference"><a href="#cite_note-ChandraBlog_2013-22"><span class="cite-bracket">[</span>22<span class="cite-bracket">]</span></a></sup> The neutron star's gravity accelerates infalling matter to tremendous speed, and <a href="/wiki/Tidal_force" title="Tidal force">tidal forces</a> near the surface can cause <a href="/wiki/Spaghettification" title="Spaghettification">spaghettification</a>.<sup id="cite_ref-ChandraBlog_2013_22-1" class="reference"><a href="#cite_note-ChandraBlog_2013-22"><span class="cite-bracket">[</span>22<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading2"><h2 id="Properties">Properties</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=2" title="Edit section: Properties"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <style data-mw-deduplicate="TemplateStyles:r1251242444">.mw-parser-output .ambox{border:1px solid #a2a9b1;border-left:10px solid #36c;background-color:#fbfbfb;box-sizing:border-box}.mw-parser-output .ambox+link+.ambox,.mw-parser-output .ambox+link+style+.ambox,.mw-parser-output .ambox+link+link+.ambox,.mw-parser-output .ambox+.mw-empty-elt+link+.ambox,.mw-parser-output .ambox+.mw-empty-elt+link+style+.ambox,.mw-parser-output .ambox+.mw-empty-elt+link+link+.ambox{margin-top:-1px}html body.mediawiki .mw-parser-output .ambox.mbox-small-left{margin:4px 1em 4px 0;overflow:hidden;width:238px;border-collapse:collapse;font-size:88%;line-height:1.25em}.mw-parser-output .ambox-speedy{border-left:10px solid #b32424;background-color:#fee7e6}.mw-parser-output .ambox-delete{border-left:10px solid #b32424}.mw-parser-output .ambox-content{border-left:10px solid #f28500}.mw-parser-output .ambox-style{border-left:10px solid #fc3}.mw-parser-output .ambox-move{border-left:10px solid #9932cc}.mw-parser-output .ambox-protection{border-left:10px solid #a2a9b1}.mw-parser-output .ambox .mbox-text{border:none;padding:0.25em 0.5em;width:100%}.mw-parser-output .ambox .mbox-image{border:none;padding:2px 0 2px 0.5em;text-align:center}.mw-parser-output .ambox .mbox-imageright{border:none;padding:2px 0.5em 2px 0;text-align:center}.mw-parser-output .ambox .mbox-empty-cell{border:none;padding:0;width:1px}.mw-parser-output .ambox .mbox-image-div{width:52px}@media(min-width:720px){.mw-parser-output .ambox{margin:0 10%}}@media print{body.ns-0 .mw-parser-output .ambox{display:none!important}}</style><table class="box-More_citations_needed_section plainlinks metadata ambox ambox-content ambox-Refimprove" role="presentation"><tbody><tr><td class="mbox-image"><div class="mbox-image-div"><span typeof="mw:File"><a href="/wiki/File:Question_book-new.svg" class="mw-file-description"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/9/99/Question_book-new.svg/50px-Question_book-new.svg.png" decoding="async" width="50" height="39" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/9/99/Question_book-new.svg/75px-Question_book-new.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/9/99/Question_book-new.svg/100px-Question_book-new.svg.png 2x" data-file-width="512" data-file-height="399" /></a></span></div></td><td class="mbox-text"><div class="mbox-text-span">This section <b>needs additional citations for <a href="/wiki/Wikipedia:Verifiability" title="Wikipedia:Verifiability">verification</a></b>.<span class="hide-when-compact"> Please help <a href="/wiki/Special:EditPage/Neutron_star" title="Special:EditPage/Neutron star">improve this article</a> by <a href="/wiki/Help:Referencing_for_beginners" title="Help:Referencing for beginners">adding citations to reliable sources</a> in this section. Unsourced material may be challenged and removed.</span> <span class="date-container"><i>(<span class="date">May 2024</span>)</i></span><span class="hide-when-compact"><i> (<small><a href="/wiki/Help:Maintenance_template_removal" title="Help:Maintenance template removal">Learn how and when to remove this message</a></small>)</i></span></div></td></tr></tbody></table> <div class="mw-heading mw-heading3"><h3 id="Equation_of_state">Equation of state</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=3" title="Edit section: Equation of state"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>The <a href="/wiki/Equation_of_state" title="Equation of state">equation of state</a> of neutron stars is not currently known. This is because neutron stars are the second most dense known object in the universe, only less dense than black holes. The extreme density means there is no way to replicate the material on earth in laboratories, which is how equations of state for other things like ideal gases are tested. The closest neutron star is many parsecs away, meaning there is no feasible way to study it directly. While it is known neutron stars should be similar to a <a href="/wiki/Degenerate_matter#:~:text=Degenerate_gases_are_gases_composed,white_dwarfs_are_two_examples." title="Degenerate matter">degenerate gas</a>, it cannot be modeled strictly like one (as white dwarfs are) because of the extreme gravity. <a href="/wiki/General_relativity" title="General relativity">General relativity</a> must be considered for the neutron star equation of state because <a href="/wiki/Newton%27s_law_of_universal_gravitation" title="Newton's law of universal gravitation">Newtonian gravity</a> is no longer sufficient in those conditions. Effects such as <a href="/wiki/Quantum_chromodynamics" title="Quantum chromodynamics">quantum chromodynamics (QCD)</a>, <a href="/wiki/Superconductivity" title="Superconductivity">superconductivity</a>, and <a href="/wiki/Superfluidity" title="Superfluidity">superfluidity</a> must also be considered. </p><p>At the extraordinarily high densities of neutron stars, ordinary matter is squeezed to nuclear densities. Specifically, the matter ranges from nuclei embedded in a sea of electrons at low densities in the outer crust, to increasingly neutron-rich structures in the inner crust, to the extremely neutron-rich uniform matter in the outer core, and possibly exotic states of matter at high densities in the inner core.<sup id="cite_ref-:1_23-0" class="reference"><a href="#cite_note-:1-23"><span class="cite-bracket">[</span>23<span class="cite-bracket">]</span></a></sup> </p><p>Understanding the nature of the matter present in the various layers of neutron stars, and the phase transitions that occur at the boundaries of the layers is a major unsolved problem in fundamental physics. The neutron star equation of state encodes information about the structure of a neutron star and thus tells us how matter behaves at the extreme densities found inside neutron stars. Constraints on the neutron star equation of state would then provide constraints on how the <a href="/wiki/Strong_interaction" title="Strong interaction">strong force</a> of the <a href="/wiki/Standard_Model" title="Standard Model">standard model</a> works, which would have profound implications for nuclear and atomic physics. This makes neutron stars natural laboratories for probing fundamental physics. </p><p>For example, the exotic states that may be found at the cores of neutron stars are types of <a href="/wiki/QCD_matter" title="QCD matter">QCD matter</a>. At the extreme densities at the centers of neutron stars, neutrons become disrupted giving rise to a sea of quarks. This matter's equation of state is governed by the laws of <a href="/wiki/Quantum_chromodynamics" title="Quantum chromodynamics">quantum chromodynamics</a> and since QCD matter cannot be produced in any laboratory on Earth, most of the current knowledge about it is only theoretical. </p><p>Different equations of state lead to different values of observable quantities. While the equation of state is only directly relating the density and pressure, it also leads to calculating observables like the speed of sound, mass, radius, and <a href="/wiki/Love_number" title="Love number">Love numbers</a>. Because the equation of state is unknown, there are many proposed ones, such as FPS, UU, APR, L, and SLy, and it is an active area of research. Different factors can be considered when creating the equation of state such as phase transitions. </p><p>Another aspect of the equation of state is whether it is a soft or stiff equation of state. This relates to how much pressure there is at a certain energy density, and often corresponds to phase transitions. When the material is about to go through a phase transition, the pressure will tend to increase until it shifts into a more comfortable state of matter. A soft equation of state would have a gently rising pressure versus energy density while a stiff one would have a sharper rise in pressure. In neutron stars, nuclear physicists are still testing whether the equation of state should be stiff or soft, and sometimes it changes within individual equations of state depending on the phase transitions within the model. This is referred to as the equation of state stiffening or softening, depending on the previous behavior. Since it is unknown what neutron stars are made of, there is room for different phases of matter to be explored within the equation of state. </p> <div class="mw-heading mw-heading3"><h3 id="Density_and_pressure">Density and pressure</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=4" title="Edit section: Density and pressure"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size mw-halign-right" typeof="mw:File/Thumb"><a href="/wiki/File:White_dwarf_vs_neutron_star.svg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/d/df/White_dwarf_vs_neutron_star.svg/220px-White_dwarf_vs_neutron_star.svg.png" decoding="async" width="220" height="220" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/d/df/White_dwarf_vs_neutron_star.svg/330px-White_dwarf_vs_neutron_star.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/d/df/White_dwarf_vs_neutron_star.svg/440px-White_dwarf_vs_neutron_star.svg.png 2x" data-file-width="1300" data-file-height="1300" /></a><figcaption>Comparison of a 10 km radius neutron star (top left corner) and a 6000 km radius <a href="/wiki/White_dwarf" title="White dwarf">white dwarf</a>, the latter roughly the size of <a href="/wiki/Earth" title="Earth">Earth</a>.</figcaption></figure> <p>Neutron stars have overall densities of <span class="nowrap"><span data-sort-value="7017370000000000000♠"></span>3.7<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>17</sup></span> to <span class="nowrap"><span data-sort-value="7017590000000000000♠"></span>5.9<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>17</sup> kg/m<sup>3</sup></span> (<span class="nowrap"><span data-sort-value="7014260000000000000♠"></span>2.6<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>14</sup></span> to <span class="nowrap"><span data-sort-value="7014409999999999999♠"></span>4.1<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>14</sup></span> times the density of the Sun),<sup id="cite_ref-24" class="reference"><a href="#cite_note-24"><span class="cite-bracket">[</span>a<span class="cite-bracket">]</span></a></sup> which is comparable to the approximate density of an atomic nucleus of <span class="nowrap"><span data-sort-value="7017300000000000000♠"></span>3<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>17</sup> kg/m<sup>3</sup></span>.<sup id="cite_ref-25" class="reference"><a href="#cite_note-25"><span class="cite-bracket">[</span>24<span class="cite-bracket">]</span></a></sup> The density increases with depth, varying from about <span class="nowrap"><span data-sort-value="7009100000000000000♠"></span>1<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>9</sup> kg/m<sup>3</sup></span> at the crust to an estimated <span class="nowrap"><span data-sort-value="7017600000000000000♠"></span>6<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>17</sup></span> or <span class="nowrap"><span data-sort-value="7017800000000000000♠"></span>8<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>17</sup> kg/m<sup>3</sup></span> deeper inside.<sup id="cite_ref-Miller_26-0" class="reference"><a href="#cite_note-Miller-26"><span class="cite-bracket">[</span>25<span class="cite-bracket">]</span></a></sup> Pressure increases accordingly, from about <span class="nowrap"><span data-sort-value="7031320000000000000♠"></span>3.2<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>31</sup> Pa</span> (32 <a href="/wiki/Quetta-" class="mw-redirect" title="Quetta-">Q</a>Pa) at the inner crust to <span class="nowrap"><span data-sort-value="7034159999999999999♠"></span>1.6<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>34</sup> Pa</span> in the center.<sup id="cite_ref-27" class="reference"><a href="#cite_note-27"><span class="cite-bracket">[</span>26<span class="cite-bracket">]</span></a></sup> </p><p>A neutron star is so dense that one teaspoon (5 <a href="/wiki/Milliliter" class="mw-redirect" title="Milliliter">milliliters</a>) of its material would have a mass over <span class="nowrap"><span data-sort-value="7012550000000000000♠"></span>5.5<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>12</sup> kg</span>, about 900 times the mass of the <a href="/wiki/Great_Pyramid_of_Giza" title="Great Pyramid of Giza">Great Pyramid of Giza</a>.<sup id="cite_ref-28" class="reference"><a href="#cite_note-28"><span class="cite-bracket">[</span>b<span class="cite-bracket">]</span></a></sup> The entire mass of the Earth at neutron star density would fit into a sphere 305 m in diameter, about the size of the <a href="/wiki/Arecibo_Telescope" title="Arecibo Telescope">Arecibo Telescope</a>. </p><p>In popular scientific writing, neutron stars are sometimes described as macroscopic <a href="/wiki/Atomic_nucleus" title="Atomic nucleus">atomic nuclei</a>. Indeed, both states are composed of <a href="/wiki/Nucleon" title="Nucleon">nucleons</a>, and they share a similar density to within an order of magnitude. However, in other respects, neutron stars and atomic nuclei are quite different. A nucleus is held together by the <a href="/wiki/Strong_interaction" title="Strong interaction">strong interaction</a>, whereas a neutron star is held together by <a href="/wiki/Gravity" title="Gravity">gravity</a>. The density of a nucleus is uniform, while neutron stars are <a href="#Structure">predicted to consist of multiple layers</a> with varying compositions and densities.<sup id="cite_ref-29" class="reference"><a href="#cite_note-29"><span class="cite-bracket">[</span>27<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading3"><h3 id="Current_constraints">Current constraints</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=5" title="Edit section: Current constraints"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Because equations of state for neutron stars lead to different observables, such as different mass-radius relations, there are many astronomical constraints on equations of state. These come mostly from <a href="/wiki/LIGO" title="LIGO">LIGO</a>,<sup id="cite_ref-30" class="reference"><a href="#cite_note-30"><span class="cite-bracket">[</span>28<span class="cite-bracket">]</span></a></sup> which is a gravitational wave observatory, and <a href="/wiki/Neutron_Star_Interior_Composition_Explorer" title="Neutron Star Interior Composition Explorer">NICER</a>,<sup id="cite_ref-31" class="reference"><a href="#cite_note-31"><span class="cite-bracket">[</span>29<span class="cite-bracket">]</span></a></sup> which is an X-ray telescope. </p><p>NICER's observations of <a href="/wiki/Pulsar" title="Pulsar">pulsars</a> in binary systems, from which the pulsar mass and radius can be estimated, can constrain the neutron star equation of state. A 2021 measurement of the pulsar <a href="/wiki/PSR_J0740%2B6620" title="PSR J0740+6620">PSR J0740+6620</a> was able to constrain the radius of a 1.4 solar mass neutron star to <span class="nowrap"><span data-sort-value="7001123300000000000♠"></span>12.33<span style="margin-left:0.3em;"><span style="display:inline-block;margin-bottom:-0.3em;vertical-align:-0.4em;line-height:1.2em;font-size:85%;text-align:right;">+0.76<br />−0.8</span></span></span> km with 95% confidence.<sup id="cite_ref-32" class="reference"><a href="#cite_note-32"><span class="cite-bracket">[</span>30<span class="cite-bracket">]</span></a></sup> These mass-radius constraints, combined with <a href="/wiki/Chiral_perturbation_theory" title="Chiral perturbation theory">chiral effective field theory</a> calculations, tightens constraints on the neutron star equation of state.<sup id="cite_ref-:1_23-1" class="reference"><a href="#cite_note-:1-23"><span class="cite-bracket">[</span>23<span class="cite-bracket">]</span></a></sup> </p><p>Equation of state constraints from LIGO gravitational wave detections start with nuclear and atomic physics researchers, who work to propose theoretical equations of state (such as FPS, UU, APR, L, SLy, and others). The proposed equations of state can then be passed onto astrophysics researchers who run simulations of <a href="/wiki/Neutron_star_merger" title="Neutron star merger">binary neutron star mergers</a>. From these simulations, researchers can extract <a href="/wiki/Gravitational_wave" title="Gravitational wave">gravitational waveforms</a>, thus studying the relationship between the equation of state and gravitational waves emitted by binary neutron star mergers. Using these relations, one can constrain the neutron star equation of state when gravitational waves from binary neutron star mergers are observed. Past <a href="/wiki/Numerical_relativity" title="Numerical relativity">numerical relativity</a> simulations of binary neutron star mergers have found relationships between the equation of state and frequency dependent peaks of the gravitational wave signal that can be applied to <a href="/wiki/LIGO" title="LIGO">LIGO</a> detections.<sup id="cite_ref-33" class="reference"><a href="#cite_note-33"><span class="cite-bracket">[</span>31<span class="cite-bracket">]</span></a></sup> For example, the LIGO detection of the binary neutron star merger <a href="/wiki/GW170817" title="GW170817">GW170817</a> provided limits on the tidal deformability of the two neutron stars which dramatically reduced the family of allowed equations of state.<sup id="cite_ref-34" class="reference"><a href="#cite_note-34"><span class="cite-bracket">[</span>32<span class="cite-bracket">]</span></a></sup> Future gravitational wave signals with next generation detectors like <a href="/wiki/Cosmic_Explorer_(gravitational_wave_observatory)" title="Cosmic Explorer (gravitational wave observatory)">Cosmic Explorer</a> can impose further constraints.<sup id="cite_ref-35" class="reference"><a href="#cite_note-35"><span class="cite-bracket">[</span>33<span class="cite-bracket">]</span></a></sup> </p><p>When nuclear physicists are trying to understand the likelihood of their equation of state, it is good to compare with these constraints to see if it predicts neutron stars of these masses and radii.<sup id="cite_ref-36" class="reference"><a href="#cite_note-36"><span class="cite-bracket">[</span>34<span class="cite-bracket">]</span></a></sup> There is also recent work on constraining the equation of state with the speed of sound through hydrodynamics.<sup id="cite_ref-37" class="reference"><a href="#cite_note-37"><span class="cite-bracket">[</span>35<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading3"><h3 id="Tolman-Oppenheimer-Volkoff_Equation">Tolman-Oppenheimer-Volkoff Equation</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=6" title="Edit section: Tolman-Oppenheimer-Volkoff Equation"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>The <a href="/wiki/Tolman%E2%80%93Oppenheimer%E2%80%93Volkoff_equation" title="Tolman–Oppenheimer–Volkoff equation">Tolman-Oppenheimer-Volkoff (TOV) equation</a> can be used to describe a neutron star. The equation is a solution to Einstein's equations from general relativity for a spherically symmetric, time invariant metric. With a given equation of state, solving the equation leads to observables such as the mass and radius. There are many codes that numerically solve the TOV equation for a given equation of state to find the mass-radius relation and other observables for that equation of state. </p><p>The following differential equations can be solved numerically to find the neutron star observables:<sup id="cite_ref-38" class="reference"><a href="#cite_note-38"><span class="cite-bracket">[</span>36<span class="cite-bracket">]</span></a></sup> </p><p><span class="mwe-math-element"><span class="mwe-math-mathml-display mwe-math-mathml-a11y" style="display: none;"><math display="block" xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle {\frac {dp}{dr}}=-{\frac {G\epsilon (r)M(r)}{c^{2}r^{2}}}\left(1+{\frac {p(r)}{\epsilon (r)}}\right)\left(1+{\frac {4\pi r^{3}p(r)}{M(r)c^{2}}}\right)\left(1-{\frac {2GM(r)}{c^{2}r}}\right)}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mrow class="MJX-TeXAtom-ORD"> <mfrac> <mrow> <mi>d</mi> <mi>p</mi> </mrow> <mrow> <mi>d</mi> <mi>r</mi> </mrow> </mfrac> </mrow> <mo>=</mo> <mo>−</mo> <mrow class="MJX-TeXAtom-ORD"> <mfrac> <mrow> <mi>G</mi> <mi>ϵ</mi> <mo stretchy="false">(</mo> <mi>r</mi> <mo stretchy="false">)</mo> <mi>M</mi> <mo stretchy="false">(</mo> <mi>r</mi> <mo stretchy="false">)</mo> </mrow> <mrow> <msup> <mi>c</mi> <mrow class="MJX-TeXAtom-ORD"> <mn>2</mn> </mrow> </msup> <msup> <mi>r</mi> <mrow class="MJX-TeXAtom-ORD"> <mn>2</mn> </mrow> </msup> </mrow> </mfrac> </mrow> <mrow> <mo>(</mo> <mrow> <mn>1</mn> <mo>+</mo> <mrow class="MJX-TeXAtom-ORD"> <mfrac> <mrow> <mi>p</mi> <mo stretchy="false">(</mo> <mi>r</mi> <mo stretchy="false">)</mo> </mrow> <mrow> <mi>ϵ</mi> <mo stretchy="false">(</mo> <mi>r</mi> <mo stretchy="false">)</mo> </mrow> </mfrac> </mrow> </mrow> <mo>)</mo> </mrow> <mrow> <mo>(</mo> <mrow> <mn>1</mn> <mo>+</mo> <mrow class="MJX-TeXAtom-ORD"> <mfrac> <mrow> <mn>4</mn> <mi>π</mi> <msup> <mi>r</mi> <mrow class="MJX-TeXAtom-ORD"> <mn>3</mn> </mrow> </msup> <mi>p</mi> <mo stretchy="false">(</mo> <mi>r</mi> <mo stretchy="false">)</mo> </mrow> <mrow> <mi>M</mi> <mo stretchy="false">(</mo> <mi>r</mi> <mo stretchy="false">)</mo> <msup> <mi>c</mi> <mrow class="MJX-TeXAtom-ORD"> <mn>2</mn> </mrow> </msup> </mrow> </mfrac> </mrow> </mrow> <mo>)</mo> </mrow> <mrow> <mo>(</mo> <mrow> <mn>1</mn> <mo>−</mo> <mrow class="MJX-TeXAtom-ORD"> <mfrac> <mrow> <mn>2</mn> <mi>G</mi> <mi>M</mi> <mo stretchy="false">(</mo> <mi>r</mi> <mo stretchy="false">)</mo> </mrow> <mrow> <msup> <mi>c</mi> <mrow class="MJX-TeXAtom-ORD"> <mn>2</mn> </mrow> </msup> <mi>r</mi> </mrow> </mfrac> </mrow> </mrow> <mo>)</mo> </mrow> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle {\frac {dp}{dr}}=-{\frac {G\epsilon (r)M(r)}{c^{2}r^{2}}}\left(1+{\frac {p(r)}{\epsilon (r)}}\right)\left(1+{\frac {4\pi r^{3}p(r)}{M(r)c^{2}}}\right)\left(1-{\frac {2GM(r)}{c^{2}r}}\right)}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/cb03d65e54f9873ecb5b13cd04f0c03515787ec4" class="mwe-math-fallback-image-display mw-invert skin-invert" aria-hidden="true" style="vertical-align: -3.171ex; width:67.036ex; height:7.509ex;" alt="{\displaystyle {\frac {dp}{dr}}=-{\frac {G\epsilon (r)M(r)}{c^{2}r^{2}}}\left(1+{\frac {p(r)}{\epsilon (r)}}\right)\left(1+{\frac {4\pi r^{3}p(r)}{M(r)c^{2}}}\right)\left(1-{\frac {2GM(r)}{c^{2}r}}\right)}"></span> <span class="mwe-math-element"><span class="mwe-math-mathml-display mwe-math-mathml-a11y" style="display: none;"><math display="block" xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle {\frac {dM}{dr}}={\frac {4\pi }{c^{2}}}r^{2}\epsilon (r)}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mrow class="MJX-TeXAtom-ORD"> <mfrac> <mrow> <mi>d</mi> <mi>M</mi> </mrow> <mrow> <mi>d</mi> <mi>r</mi> </mrow> </mfrac> </mrow> <mo>=</mo> <mrow class="MJX-TeXAtom-ORD"> <mfrac> <mrow> <mn>4</mn> <mi>π</mi> </mrow> <msup> <mi>c</mi> <mrow class="MJX-TeXAtom-ORD"> <mn>2</mn> </mrow> </msup> </mfrac> </mrow> <msup> <mi>r</mi> <mrow class="MJX-TeXAtom-ORD"> <mn>2</mn> </mrow> </msup> <mi>ϵ</mi> <mo stretchy="false">(</mo> <mi>r</mi> <mo stretchy="false">)</mo> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle {\frac {dM}{dr}}={\frac {4\pi }{c^{2}}}r^{2}\epsilon (r)}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/4eaf94434c86ab60501f877862ccec4c92faf386" class="mwe-math-fallback-image-display mw-invert skin-invert" aria-hidden="true" style="vertical-align: -2.171ex; width:16.828ex; height:5.676ex;" alt="{\displaystyle {\frac {dM}{dr}}={\frac {4\pi }{c^{2}}}r^{2}\epsilon (r)}"></span> </p><p>where <span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle G}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>G</mi> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle G}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/f5f3c8921a3b352de45446a6789b104458c9f90b" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.338ex; width:1.827ex; height:2.176ex;" alt="{\displaystyle G}"></span> is the gravitational constant, <span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle p(r)}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>p</mi> <mo stretchy="false">(</mo> <mi>r</mi> <mo stretchy="false">)</mo> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle p(r)}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/62a0b6c3f80917fa2e46f00b9bcf4a71b37bbec3" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.838ex; margin-left: -0.089ex; width:4.117ex; height:2.843ex;" alt="{\displaystyle p(r)}"></span> is the pressure, <span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle \epsilon (r)}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>ϵ</mi> <mo stretchy="false">(</mo> <mi>r</mi> <mo stretchy="false">)</mo> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle \epsilon (r)}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/f3ff1d8343db9bc239e92c829863d459a97d1d09" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.838ex; width:3.802ex; height:2.843ex;" alt="{\displaystyle \epsilon (r)}"></span> is the energy density (found from the equation of state), and <span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle c}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>c</mi> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle c}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/86a67b81c2de995bd608d5b2df50cd8cd7d92455" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.338ex; width:1.007ex; height:1.676ex;" alt="{\displaystyle c}"></span> is the speed of light. </p> <div class="mw-heading mw-heading3"><h3 id="Mass-Radius_relation">Mass-Radius relation</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=7" title="Edit section: Mass-Radius relation"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Using the TOV equations and an equation of state, a mass-radius curve can be found. The idea is that for the correct equation of state, every neutron star that could possibly exist would lie along that curve. This is one of the ways equations of state can be constrained by astronomical observations. To create these curves, one must solve the TOV equations for different central densities. For each central density, you numerically solve the mass and pressure equations until the pressure goes to zero, which is the outside of the star. Each solution gives a corresponding mass and radius for that central density. </p><p>Mass-radius curves determine what the maximum mass is for a given equation of state. Through most of the mass-radius curve, each radius corresponds to a unique mass value. At a certain point, the curve will reach a maximum and start going back down, leading to repeated mass values for different radii. This maximum point is what is known as the maximum mass. Beyond that mass, the star will no longer be stable, i.e. no longer be able to hold itself up against the force of gravity, and would collapse into a black hole. Since each equation of state leads to a different mass-radius curve, they also lead to a unique maximum mass value. The maximum mass value is unknown as long as the equation of state remains unknown. </p><p>This is very important when it comes to constraining the equation of state. Oppenheimer and Volkoff came up with the <a href="/wiki/Tolman%E2%80%93Oppenheimer%E2%80%93Volkoff_limit" title="Tolman–Oppenheimer–Volkoff limit">Tolman-Oppenheimer-Volkoff limit</a> using a degenerate gas equation of state with the TOV equations that was ~0.7 Solar masses. Since the neutron stars that have been observed are more massive than that, that maximum mass was discarded. The most recent massive neutron star that was observed was <a href="/wiki/PSR_J0952%E2%80%930607" title="PSR J0952–0607">PSR J0952-0607</a> which was <span class="nowrap"><span data-sort-value="7000235000000000000♠"></span>2.35<span style="margin-left:0.3em;margin-right:0.15em;">±</span>0.17</span> solar masses. Any equation of state with a mass less than that would not predict that star and thus is much less likely to be correct. </p><p>An interesting phenomenon in this area of astrophysics relating to the maximum mass of neutron stars is what is called the "mass gap". The mass gap refers to a range of masses from roughly 2-5 solar masses where very few compact objects were observed. This range is based on the current assumed maximum mass of neutron stars (~2 solar masses) and the minimum black hole mass (~5 solar masses).<sup id="cite_ref-39" class="reference"><a href="#cite_note-39"><span class="cite-bracket">[</span>37<span class="cite-bracket">]</span></a></sup> Recently, some objects have been discovered that fall in that mass gap from gravitational wave detections. If the true maximum mass of neutron stars was known, it would help characterize compact objects in that mass range as either neutron stars or black holes. </p> <div class="mw-heading mw-heading3"><h3 id="I-Love-Q_Relations">I-Love-Q Relations</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=8" title="Edit section: I-Love-Q Relations"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>There are three more properties of neutron stars that are dependent on the equation of state but can also be astronomically observed: the <a href="/wiki/Moment_of_inertia" title="Moment of inertia">moment of inertia</a>, the <a href="/wiki/Quadrupole_moment" class="mw-redirect" title="Quadrupole moment">quadrupole moment</a>, and the <a href="/wiki/Love_number" title="Love number">Love number</a>. The moment of inertia of a neutron star describes how fast the star can rotate at a fixed spin momentum. The quadrupole moment of a neutron star specifies how much that star is deformed out of its spherical shape. The Love number of the neutron star represents how easy or difficult it is to deform the star due to <a href="/wiki/Tidal_force" title="Tidal force">tidal forces</a>, typically important in binary systems. </p><p>While these properties depend on the material of the star and therefore on the equation of state, there is a relation between these three quantities that is independent of the equation of state. This relation assumes slowly and uniformly rotating stars and uses general relativity to derive the relation. While this relation would not be able to add constraints to the equation of state, since it is independent of the equation of state, it does have other applications. If one of these three quantities can be measured for a particular neutron star, this relation can be used to find the other two. In addition, this relation can be used to break the degeneracies in detections by gravitational wave detectors of the quadrupole moment and spin, allowing the average spin to be determined within a certain confidence level.<sup id="cite_ref-40" class="reference"><a href="#cite_note-40"><span class="cite-bracket">[</span>38<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading3"><h3 id="Temperature">Temperature</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=9" title="Edit section: Temperature"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>The temperature inside a newly formed neutron star is from around <span class="nowrap"><span data-sort-value="7011100000000000000♠"></span>10<sup>11</sup></span> to <span class="nowrap"><span data-sort-value="7012100000000000000♠"></span>10<sup>12</sup> <a href="/wiki/Kelvin" title="Kelvin">kelvin</a></span>.<sup id="cite_ref-Miller_26-1" class="reference"><a href="#cite_note-Miller-26"><span class="cite-bracket">[</span>25<span class="cite-bracket">]</span></a></sup> However, the huge number of <a href="/wiki/Neutrino" title="Neutrino">neutrinos</a> it emits carries away so much energy that the temperature of an isolated neutron star falls within a few years to around <span class="nowrap"><span data-sort-value="7006100000000000000♠"></span>10<sup>6</sup> kelvin</span>.<sup id="cite_ref-Miller_26-2" class="reference"><a href="#cite_note-Miller-26"><span class="cite-bracket">[</span>25<span class="cite-bracket">]</span></a></sup> At this lower temperature, most of the light generated by a neutron star is in X-rays. </p><p>Some researchers have proposed a neutron star classification system using <a href="/wiki/Roman_numerals" title="Roman numerals">Roman numerals</a> (not to be confused with the <a href="/wiki/Stellar_classification" title="Stellar classification">Yerkes luminosity classes</a> for non-degenerate stars) to sort neutron stars by their mass and cooling rates: type I for neutron stars with low mass and cooling rates, type II for neutron stars with higher mass and cooling rates, and a proposed type III for neutron stars with even higher mass, approaching 2 <var>M</var><sub>☉</sub>, and with higher cooling rates and possibly candidates for <a href="/wiki/Exotic_star" title="Exotic star">exotic stars</a>.<sup id="cite_ref-41" class="reference"><a href="#cite_note-41"><span class="cite-bracket">[</span>39<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading3"><h3 id="Magnetic_field">Magnetic field</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=10" title="Edit section: Magnetic field"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>The magnetic field strength on the surface of neutron stars ranges from <abbr title="circa">c.</abbr><span style="white-space:nowrap;"> <span class="nowrap"><span data-sort-value="7004100000000000000♠"></span>10<sup>4</sup></span></span> to <span class="nowrap"><span data-sort-value="7011100000000000000♠"></span>10<sup>11</sup></span> <a href="/wiki/Tesla_(unit)" title="Tesla (unit)">tesla</a> (T).<sup id="cite_ref-reisenegger_42-0" class="reference"><a href="#cite_note-reisenegger-42"><span class="cite-bracket">[</span>40<span class="cite-bracket">]</span></a></sup> These are orders of magnitude higher than in any other object: for comparison, a continuous 16 T field has been achieved in the laboratory and is sufficient to levitate a living frog due to <a href="/wiki/Diamagnetic_levitation" class="mw-redirect" title="Diamagnetic levitation">diamagnetic levitation</a>. Variations in magnetic field strengths are most likely the main factor that allows different types of neutron stars to be distinguished by their spectra, and explains the periodicity of pulsars.<sup id="cite_ref-reisenegger_42-1" class="reference"><a href="#cite_note-reisenegger-42"><span class="cite-bracket">[</span>40<span class="cite-bracket">]</span></a></sup> </p><p>The neutron stars known as <a href="/wiki/Magnetar" title="Magnetar">magnetars</a> have the strongest magnetic fields, in the range of <span class="nowrap"><span data-sort-value="7008100000000000000♠"></span>10<sup>8</sup></span> to <span class="nowrap"><span data-sort-value="7011100000000000000♠"></span>10<sup>11</sup> T</span>,<sup id="cite_ref-mcgill_43-0" class="reference"><a href="#cite_note-mcgill-43"><span class="cite-bracket">[</span>41<span class="cite-bracket">]</span></a></sup> and have become the widely accepted hypothesis for neutron star types <a href="/wiki/Soft_gamma_repeater" title="Soft gamma repeater">soft gamma repeaters</a> (SGRs)<sup id="cite_ref-sa_44-0" class="reference"><a href="#cite_note-sa-44"><span class="cite-bracket">[</span>42<span class="cite-bracket">]</span></a></sup> and <a href="/wiki/Anomalous_X-ray_pulsar" title="Anomalous X-ray pulsar">anomalous X-ray pulsars</a> (AXPs).<sup id="cite_ref-45" class="reference"><a href="#cite_note-45"><span class="cite-bracket">[</span>43<span class="cite-bracket">]</span></a></sup> The magnetic <a href="/wiki/Energy_density" title="Energy density">energy density</a> of a <span class="nowrap"><span data-sort-value="7008100000000000000♠"></span>10<sup>8</sup> T</span> field is extreme, greatly exceeding the <a href="/wiki/Theoretical_total_mass-energy" class="mw-redirect" title="Theoretical total mass-energy">mass-energy</a> density of ordinary matter.<sup id="cite_ref-47" class="reference"><a href="#cite_note-47"><span class="cite-bracket">[</span>c<span class="cite-bracket">]</span></a></sup> Fields of this strength are able to <a href="/wiki/Vacuum_polarization" title="Vacuum polarization">polarize the vacuum</a> to the point that the vacuum becomes <a href="/wiki/Birefringent" class="mw-redirect" title="Birefringent">birefringent</a>. Photons can merge or split in two, and virtual particle-antiparticle pairs are produced. The field changes electron energy levels and atoms are forced into thin cylinders. Unlike in an ordinary pulsar, magnetar spin-down can be directly powered by its magnetic field, and the magnetic field is strong enough to stress the crust to the point of fracture. Fractures of the crust cause <a href="/wiki/Starquake_(astrophysics)#Starquake" class="mw-redirect" title="Starquake (astrophysics)">starquakes</a>, observed as extremely luminous millisecond hard gamma ray bursts. The fireball is trapped by the magnetic field, and comes in and out of view when the star rotates, which is observed as a periodic soft gamma repeater (SGR) emission with a period of 5–8 seconds and which lasts for a few minutes.<sup id="cite_ref-48" class="reference"><a href="#cite_note-48"><span class="cite-bracket">[</span>45<span class="cite-bracket">]</span></a></sup> </p><p>The origins of the strong magnetic field are as yet unclear.<sup id="cite_ref-reisenegger_42-2" class="reference"><a href="#cite_note-reisenegger-42"><span class="cite-bracket">[</span>40<span class="cite-bracket">]</span></a></sup> One hypothesis is that of "flux freezing", or conservation of the original <a href="/wiki/Magnetic_flux" title="Magnetic flux">magnetic flux</a> during the formation of the neutron star.<sup id="cite_ref-reisenegger_42-3" class="reference"><a href="#cite_note-reisenegger-42"><span class="cite-bracket">[</span>40<span class="cite-bracket">]</span></a></sup> If an object has a certain magnetic flux over its surface area, and that area shrinks to a smaller area, but the magnetic flux is conserved, then the <a href="/wiki/Magnetic_field" title="Magnetic field">magnetic field</a> would correspondingly increase. Likewise, a collapsing star begins with a much larger surface area than the resulting neutron star, and conservation of magnetic flux would result in a far stronger magnetic field. However, this simple explanation does not fully explain magnetic field strengths of neutron stars.<sup id="cite_ref-reisenegger_42-4" class="reference"><a href="#cite_note-reisenegger-42"><span class="cite-bracket">[</span>40<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading3"><h3 id="Gravity">Gravity</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=11" title="Edit section: Gravity"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236090951"><div role="note" class="hatnote navigation-not-searchable">See also: <a href="/wiki/Tolman%E2%80%93Oppenheimer%E2%80%93Volkoff_equation" title="Tolman–Oppenheimer–Volkoff equation">Tolman–Oppenheimer–Volkoff equation</a> and <a href="/wiki/White_dwarf#Mass–radius_relationship" title="White dwarf">White dwarf § Mass–radius relationship</a></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Neutronstar_2Rs.svg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/a/a3/Neutronstar_2Rs.svg/220px-Neutronstar_2Rs.svg.png" decoding="async" width="220" height="165" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/a/a3/Neutronstar_2Rs.svg/330px-Neutronstar_2Rs.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/a/a3/Neutronstar_2Rs.svg/440px-Neutronstar_2Rs.svg.png 2x" data-file-width="1024" data-file-height="768" /></a><figcaption>Gravitational light deflection at a neutron star. Due to relativistic light deflection over half the surface is visible (each grid patch represents 30 by 30 degrees).<sup id="cite_ref-Zahn_49-0" class="reference"><a href="#cite_note-Zahn-49"><span class="cite-bracket">[</span>46<span class="cite-bracket">]</span></a></sup> In <a href="/wiki/Geometrized_unit_system" title="Geometrized unit system">natural units</a>, this star's mass is 1 and its radius is 4, or twice its <a href="/wiki/Schwarzschild_radius" title="Schwarzschild radius">Schwarzschild radius</a>.<sup id="cite_ref-Zahn_49-1" class="reference"><a href="#cite_note-Zahn-49"><span class="cite-bracket">[</span>46<span class="cite-bracket">]</span></a></sup></figcaption></figure> <p>The gravitational field at a neutron star's surface is about <span class="nowrap"><span data-sort-value="7011200000000000000♠"></span>2<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>11</sup></span> times <a href="/wiki/Standard_gravity" title="Standard gravity">stronger than on Earth</a>, at around <span class="nowrap"><span data-sort-value="7012200000000000000♠"></span>2.0<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>12</sup> m/s<sup>2</sup></span>.<sup id="cite_ref-50" class="reference"><a href="#cite_note-50"><span class="cite-bracket">[</span>47<span class="cite-bracket">]</span></a></sup> Such a strong gravitational field acts as a <a href="/wiki/Gravitational_lens" title="Gravitational lens">gravitational lens</a> and bends the radiation emitted by the neutron star such that parts of the normally invisible rear surface become visible.<sup id="cite_ref-Zahn_49-2" class="reference"><a href="#cite_note-Zahn-49"><span class="cite-bracket">[</span>46<span class="cite-bracket">]</span></a></sup> If the radius of the neutron star is 3<i>GM</i>/<i>c</i><sup>2</sup> or less, then the photons may be <a href="/wiki/Photon_sphere" title="Photon sphere">trapped in an orbit</a>, thus making the whole surface of that neutron star visible from a single vantage point, along with destabilizing photon orbits at or below the 1 radius distance of the star. </p><p>A fraction of the mass of a star that collapses to form a neutron star is released in the supernova explosion from which it forms (from the law of mass–energy equivalence, <span class="nowrap"><i>E</i> = <i>mc</i><sup>2</sup></span>). The energy comes from the <a href="/wiki/Gravitational_binding_energy" title="Gravitational binding energy">gravitational binding energy</a> of a neutron star. </p><p>Hence, the gravitational force of a typical neutron star is huge. If an object were to fall from a height of one meter on a neutron star 12 kilometers in radius, it would reach the ground at around 1,400 kilometers per second.<sup id="cite_ref-51" class="reference"><a href="#cite_note-51"><span class="cite-bracket">[</span>48<span class="cite-bracket">]</span></a></sup> However, even before impact, the <a href="/wiki/Tidal_force" title="Tidal force">tidal force</a> would cause <a href="/wiki/Spaghettification" title="Spaghettification">spaghettification</a>, breaking any sort of an ordinary object into a stream of material. </p><p>Because of the enormous gravity, <a href="/wiki/Time_dilation" title="Time dilation">time dilation</a> between a neutron star and Earth is significant. For example, eight years could pass on the surface of a neutron star, yet ten years would have passed on Earth, not including the time-dilation effect of the star's very rapid rotation.<sup id="cite_ref-52" class="reference"><a href="#cite_note-52"><span class="cite-bracket">[</span>49<span class="cite-bracket">]</span></a></sup> </p><p>Neutron star relativistic equations of state describe the relation of radius vs. mass for various models.<sup id="cite_ref-53" class="reference"><a href="#cite_note-53"><span class="cite-bracket">[</span>50<span class="cite-bracket">]</span></a></sup> The most likely radii for a given neutron star mass are bracketed by models AP4 (smallest radius) and MS2 (largest radius). <i>E</i><sub>B</sub> is the ratio of gravitational binding energy mass equivalent to the observed neutron star gravitational mass of <i>M</i> kilograms with radius <i>R</i> meters,<sup id="cite_ref-54" class="reference"><a href="#cite_note-54"><span class="cite-bracket">[</span>51<span class="cite-bracket">]</span></a></sup> <span class="mwe-math-element"><span class="mwe-math-mathml-display mwe-math-mathml-a11y" style="display: none;"><math display="block" xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle E_{\text{B}}={\frac {0.60\,\beta }{1-{\frac {\beta }{2}}}}}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <msub> <mi>E</mi> <mrow class="MJX-TeXAtom-ORD"> <mtext>B</mtext> </mrow> </msub> <mo>=</mo> <mrow class="MJX-TeXAtom-ORD"> <mfrac> <mrow> <mn>0.60</mn> <mspace width="thinmathspace" /> <mi>β</mi> </mrow> <mrow> <mn>1</mn> <mo>−</mo> <mrow class="MJX-TeXAtom-ORD"> <mfrac> <mi>β</mi> <mn>2</mn> </mfrac> </mrow> </mrow> </mfrac> </mrow> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle E_{\text{B}}={\frac {0.60\,\beta }{1-{\frac {\beta }{2}}}}}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/185e07db3d0a4d6f51ed3dfea475485392be08f2" class="mwe-math-fallback-image-display mw-invert skin-invert" aria-hidden="true" style="vertical-align: -3.838ex; width:12.899ex; height:7.343ex;" alt="{\displaystyle E_{\text{B}}={\frac {0.60\,\beta }{1-{\frac {\beta }{2}}}}}"></span><span class="mwe-math-element"><span class="mwe-math-mathml-display mwe-math-mathml-a11y" style="display: none;"><math display="block" xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle \beta \ =G\,M/R\,{c}^{2}}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>β</mi> <mtext> </mtext> <mo>=</mo> <mi>G</mi> <mspace width="thinmathspace" /> <mi>M</mi> <mrow class="MJX-TeXAtom-ORD"> <mo>/</mo> </mrow> <mi>R</mi> <mspace width="thinmathspace" /> <msup> <mrow class="MJX-TeXAtom-ORD"> <mi>c</mi> </mrow> <mrow class="MJX-TeXAtom-ORD"> <mn>2</mn> </mrow> </msup> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle \beta \ =G\,M/R\,{c}^{2}}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/abd3535cbfb97206df29ff5549da5eee8cb91bf0" class="mwe-math-fallback-image-display mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.838ex; width:15.042ex; height:3.176ex;" alt="{\displaystyle \beta \ =G\,M/R\,{c}^{2}}"></span> Given current values </p> <ul><li><span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle G=6.67408\times 10^{-11}\,{\text{m}}^{3}{\text{kg}}^{-1}{\text{s}}^{-2}}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>G</mi> <mo>=</mo> <mn>6.67408</mn> <mo>×</mo> <msup> <mn>10</mn> <mrow class="MJX-TeXAtom-ORD"> <mo>−</mo> <mn>11</mn> </mrow> </msup> <mspace width="thinmathspace" /> <msup> <mrow class="MJX-TeXAtom-ORD"> <mtext>m</mtext> </mrow> <mrow class="MJX-TeXAtom-ORD"> <mn>3</mn> </mrow> </msup> <msup> <mrow class="MJX-TeXAtom-ORD"> <mtext>kg</mtext> </mrow> <mrow class="MJX-TeXAtom-ORD"> <mo>−</mo> <mn>1</mn> </mrow> </msup> <msup> <mrow class="MJX-TeXAtom-ORD"> <mtext>s</mtext> </mrow> <mrow class="MJX-TeXAtom-ORD"> <mo>−</mo> <mn>2</mn> </mrow> </msup> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle G=6.67408\times 10^{-11}\,{\text{m}}^{3}{\text{kg}}^{-1}{\text{s}}^{-2}}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/cfb220c966d095f02289f8977286852b4b1379eb" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.671ex; width:32.216ex; height:3.009ex;" alt="{\displaystyle G=6.67408\times 10^{-11}\,{\text{m}}^{3}{\text{kg}}^{-1}{\text{s}}^{-2}}"></span><sup id="cite_ref-CODATA_2014_55-0" class="reference"><a href="#cite_note-CODATA_2014-55"><span class="cite-bracket">[</span>52<span class="cite-bracket">]</span></a></sup></li> <li><span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle c=2.99792458\times 10^{8}\,{\text{m}}/{\text{s}}}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>c</mi> <mo>=</mo> <mn>2.99792458</mn> <mo>×</mo> <msup> <mn>10</mn> <mrow class="MJX-TeXAtom-ORD"> <mn>8</mn> </mrow> </msup> <mspace width="thinmathspace" /> <mrow class="MJX-TeXAtom-ORD"> <mtext>m</mtext> </mrow> <mrow class="MJX-TeXAtom-ORD"> <mo>/</mo> </mrow> <mrow class="MJX-TeXAtom-ORD"> <mtext>s</mtext> </mrow> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle c=2.99792458\times 10^{8}\,{\text{m}}/{\text{s}}}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/1be6155b8c644c1dca0370871f7666841e3a87b7" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.838ex; width:25.835ex; height:3.176ex;" alt="{\displaystyle c=2.99792458\times 10^{8}\,{\text{m}}/{\text{s}}}"></span><sup id="cite_ref-CODATA_2014_55-1" class="reference"><a href="#cite_note-CODATA_2014-55"><span class="cite-bracket">[</span>52<span class="cite-bracket">]</span></a></sup></li> <li><span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle M_{\odot }=1.98855\times 10^{30}\,{\text{kg}}}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <msub> <mi>M</mi> <mrow class="MJX-TeXAtom-ORD"> <mo>⊙</mo> </mrow> </msub> <mo>=</mo> <mn>1.98855</mn> <mo>×</mo> <msup> <mn>10</mn> <mrow class="MJX-TeXAtom-ORD"> <mn>30</mn> </mrow> </msup> <mspace width="thinmathspace" /> <mrow class="MJX-TeXAtom-ORD"> <mtext>kg</mtext> </mrow> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle M_{\odot }=1.98855\times 10^{30}\,{\text{kg}}}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/a967ceab7c7010abf75330d932b69a07843300b1" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.671ex; width:24.303ex; height:3.009ex;" alt="{\displaystyle M_{\odot }=1.98855\times 10^{30}\,{\text{kg}}}"></span></li></ul> <p>and star masses "M" commonly reported as multiples of one solar mass, <span class="mwe-math-element"><span class="mwe-math-mathml-display mwe-math-mathml-a11y" style="display: none;"><math display="block" xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle M_{x}={\frac {M}{M_{\odot }}}}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <msub> <mi>M</mi> <mrow class="MJX-TeXAtom-ORD"> <mi>x</mi> </mrow> </msub> <mo>=</mo> <mrow class="MJX-TeXAtom-ORD"> <mfrac> <mi>M</mi> <msub> <mi>M</mi> <mrow class="MJX-TeXAtom-ORD"> <mo>⊙</mo> </mrow> </msub> </mfrac> </mrow> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle M_{x}={\frac {M}{M_{\odot }}}}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/48c7f4bf3ece0019c0a846e540e65470682df057" class="mwe-math-fallback-image-display mw-invert skin-invert" aria-hidden="true" style="vertical-align: -2.338ex; width:11.126ex; height:5.676ex;" alt="{\displaystyle M_{x}={\frac {M}{M_{\odot }}}}"></span> then the relativistic fractional binding energy of a neutron star is <span class="mwe-math-element"><span class="mwe-math-mathml-display mwe-math-mathml-a11y" style="display: none;"><math display="block" xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle E_{\text{B}}={\frac {886.0\,M_{x}}{R_{\left[{\text{in meters}}\right]}-738.3\,M_{x}}}}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <msub> <mi>E</mi> <mrow class="MJX-TeXAtom-ORD"> <mtext>B</mtext> </mrow> </msub> <mo>=</mo> <mrow class="MJX-TeXAtom-ORD"> <mfrac> <mrow> <mn>886.0</mn> <mspace width="thinmathspace" /> <msub> <mi>M</mi> <mrow class="MJX-TeXAtom-ORD"> <mi>x</mi> </mrow> </msub> </mrow> <mrow> <msub> <mi>R</mi> <mrow class="MJX-TeXAtom-ORD"> <mrow> <mo>[</mo> <mrow class="MJX-TeXAtom-ORD"> <mtext>in meters</mtext> </mrow> <mo>]</mo> </mrow> </mrow> </msub> <mo>−</mo> <mn>738.3</mn> <mspace width="thinmathspace" /> <msub> <mi>M</mi> <mrow class="MJX-TeXAtom-ORD"> <mi>x</mi> </mrow> </msub> </mrow> </mfrac> </mrow> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle E_{\text{B}}={\frac {886.0\,M_{x}}{R_{\left[{\text{in meters}}\right]}-738.3\,M_{x}}}}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/558558683ac32f47013ae0681a73d48f399f6202" class="mwe-math-fallback-image-display mw-invert skin-invert" aria-hidden="true" style="vertical-align: -2.671ex; width:28.62ex; height:6.009ex;" alt="{\displaystyle E_{\text{B}}={\frac {886.0\,M_{x}}{R_{\left[{\text{in meters}}\right]}-738.3\,M_{x}}}}"></span> </p><p>A 2 <var>M</var><sub>☉</sub> neutron star would not be more compact than 10,970 meters radius (AP4 model). Its mass fraction gravitational binding energy would then be 0.187, −18.7% (exothermic). This is not near 0.6/2 = 0.3, −30%. </p> <div class="mw-heading mw-heading2"><h2 id="Structure">Structure</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=12" title="Edit section: Structure"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Neutron_star_cross_section.svg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/9/9e/Neutron_star_cross_section.svg/220px-Neutron_star_cross_section.svg.png" decoding="async" width="220" height="127" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/9/9e/Neutron_star_cross_section.svg/330px-Neutron_star_cross_section.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/9/9e/Neutron_star_cross_section.svg/440px-Neutron_star_cross_section.svg.png 2x" data-file-width="888" data-file-height="511" /></a><figcaption>Cross-section of neutron star. Densities are in terms of <i>ρ<sub>0</sub></i> the saturation <a href="/wiki/Nuclear_density" title="Nuclear density">nuclear matter density</a>, where nucleons begin to touch.</figcaption></figure> <p>Current understanding of the structure of neutron stars is defined by existing mathematical models, but it might be possible to infer some details through studies of <a href="/wiki/Neutron-star_oscillations" class="mw-redirect" title="Neutron-star oscillations">neutron-star oscillations</a>. <a href="/wiki/Asteroseismology" title="Asteroseismology">Asteroseismology</a>, a study applied to ordinary stars, can reveal the inner structure of neutron stars by analyzing observed <a href="/wiki/Frequency_spectrum" class="mw-redirect" title="Frequency spectrum">spectra</a> of stellar oscillations.<sup id="cite_ref-Haensel_21-1" class="reference"><a href="#cite_note-Haensel-21"><span class="cite-bracket">[</span>21<span class="cite-bracket">]</span></a></sup> </p><p>Current models indicate that matter at the surface of a neutron star is composed of ordinary <a href="/wiki/Atomic_nucleus" title="Atomic nucleus">atomic nuclei</a> crushed into a solid lattice with a sea of <a href="/wiki/Electron" title="Electron">electrons</a> flowing through the gaps between them. It is possible that the nuclei at the surface are <a href="/wiki/Iron" title="Iron">iron</a>, due to iron's high <a href="/wiki/Binding_energy" title="Binding energy">binding energy</a> per nucleon.<sup id="cite_ref-Surface_56-0" class="reference"><a href="#cite_note-Surface-56"><span class="cite-bracket">[</span>53<span class="cite-bracket">]</span></a></sup> It is also possible that heavy elements, such as iron, simply sink beneath the surface, leaving only light nuclei like <a href="/wiki/Helium" title="Helium">helium</a> and <a href="/wiki/Hydrogen" title="Hydrogen">hydrogen</a>.<sup id="cite_ref-Surface_56-1" class="reference"><a href="#cite_note-Surface-56"><span class="cite-bracket">[</span>53<span class="cite-bracket">]</span></a></sup> If the surface temperature exceeds <span class="nowrap"><span data-sort-value="7006100000000000000♠"></span>10<sup>6</sup> kelvins</span> (as in the case of a young pulsar), the surface should be fluid instead of the solid phase that might exist in cooler neutron stars (temperature <<span class="nowrap"><span data-sort-value="7006100000000000000♠"></span>10<sup>6</sup> kelvins</span>).<sup id="cite_ref-Surface_56-2" class="reference"><a href="#cite_note-Surface-56"><span class="cite-bracket">[</span>53<span class="cite-bracket">]</span></a></sup> </p><p>The "atmosphere" of a neutron star is hypothesized to be at most several micrometers thick, and its dynamics are fully controlled by the neutron star's magnetic field. Below the atmosphere one encounters a solid "crust". This crust is extremely hard and very smooth (with maximum surface irregularities on the order of millimeters or less), due to the extreme gravitational field.<sup id="cite_ref-57" class="reference"><a href="#cite_note-57"><span class="cite-bracket">[</span>54<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-mt-ls_58-0" class="reference"><a href="#cite_note-mt-ls-58"><span class="cite-bracket">[</span>55<span class="cite-bracket">]</span></a></sup> </p><p>Proceeding inward, one encounters nuclei with ever-increasing numbers of neutrons; such nuclei would decay quickly on Earth, but are kept stable by tremendous pressures. As this process continues at increasing depths, the <a href="/wiki/Neutron_drip_line" class="mw-redirect" title="Neutron drip line">neutron drip</a> becomes overwhelming, and the concentration of free neutrons increases rapidly. </p><p>After a <a href="/wiki/Supernova" title="Supernova">supernova</a> explosion of a <a href="/wiki/Supergiant" title="Supergiant">supergiant</a> star, neutron stars are born from the remnants. A neutron star is composed mostly of <a href="/wiki/Neutron" title="Neutron">neutrons</a> (neutral particles) and contains a small fraction of <a href="/wiki/Proton" title="Proton">protons</a> (positively charged particles) and <a href="/wiki/Electron" title="Electron">electrons</a> (negatively charged particles), as well as nuclei. In the extreme density of a neutron star, many neutrons are free neutrons, meaning they are not bound in atomic nuclei and move freely within the star's dense matter, especially in the densest regions of the star—the inner crust and core. Over the star's lifetime, as its density increases, the energy of the electrons also increases, which generates more neutrons.<sup id="cite_ref-burrows_59-0" class="reference"><a href="#cite_note-burrows-59"><span class="cite-bracket">[</span>56<span class="cite-bracket">]</span></a></sup> </p><p>In neutron stars, the neutron drip is the transition point where nuclei become so neutron-rich that they can no longer hold additional neutrons, leading to a sea of free neutrons being formed. The sea of neutrons formed after neutron drip provides additional pressure support, which helps maintain the star's structural integrity and prevents gravitational collapse. The neutron drip takes place within the inner crust of the neutron star and starts when the density becomes so high that nuclei can no longer hold additional neutrons.<sup id="cite_ref-sorlin2008_60-0" class="reference"><a href="#cite_note-sorlin2008-60"><span class="cite-bracket">[</span>57<span class="cite-bracket">]</span></a></sup> </p><p>At the beginning of the neutron drip, the pressure in the star from neutrons, electrons, and the total pressure is roughly equal. As the density of the neutron star increases, the nuclei break down, and the neutron pressure of the star becomes dominant. When the density reaches a point where nuclei touch and subsequently merge, they form a fluid of neutrons with a sprinkle of electrons and protons. This transition marks the neutron drip, where the dominant pressure in the neutron star shifts from degenerate electrons to neutrons. </p><p>At very high densities, the neutron pressure becomes the primary pressure holding up the star, with neutrons being non-relativistic (moving slower than the speed of light) and extremely compressed. However, at extremely high densities, neutrons begin to move at relativistic speeds (close to the speed of light). These high speeds significantly increase the star's overall pressure, altering the star's equilibrium state, and potentially leading to the formation of exotic states of matter. </p><p>In that region, there are nuclei, free electrons, and free neutrons. The nuclei become increasingly small (gravity and pressure overwhelming the <a href="/wiki/Strong_force" class="mw-redirect" title="Strong force">strong force</a>) until the core is reached, by definition the point where mostly neutrons exist. The expected hierarchy of phases of nuclear matter in the inner crust has been characterized as "<a href="/wiki/Nuclear_pasta" title="Nuclear pasta">nuclear pasta</a>", with fewer voids and larger structures towards higher pressures.<sup id="cite_ref-61" class="reference"><a href="#cite_note-61"><span class="cite-bracket">[</span>58<span class="cite-bracket">]</span></a></sup> The composition of the superdense matter in the core remains uncertain. One model describes the core as <a href="/wiki/Superfluid" class="mw-redirect" title="Superfluid">superfluid</a> <a href="/wiki/Degenerate_matter#Neutron_degeneracy" title="Degenerate matter">neutron-degenerate matter</a> (mostly neutrons, with some protons and electrons). More exotic forms of matter are possible, including degenerate <a href="/wiki/Strange_matter" title="Strange matter">strange matter</a> (containing <a href="/wiki/Strange_quark" title="Strange quark">strange quarks</a> in addition to <a href="/wiki/Up_quark" title="Up quark">up</a> and <a href="/wiki/Down_quark" title="Down quark">down quarks</a>), matter containing high-energy <a href="/wiki/Pion" title="Pion">pions</a> and <a href="/wiki/Kaon" title="Kaon">kaons</a> in addition to neutrons,<sup id="cite_ref-Haensel_21-2" class="reference"><a href="#cite_note-Haensel-21"><span class="cite-bracket">[</span>21<span class="cite-bracket">]</span></a></sup> or ultra-dense <a href="/wiki/Degenerate_matter#Quark_degeneracy" title="Degenerate matter">quark-degenerate matter</a>. </p> <div class="mw-heading mw-heading2"><h2 id="Radiation">Radiation</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=13" title="Edit section: Radiation"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><span><video id="mwe_player_3" poster="//upload.wikimedia.org/wikipedia/commons/thumb/b/b7/Pulsar_anim.ogv/220px--Pulsar_anim.ogv.jpg" controls="" preload="none" data-mw-tmh="" class="mw-file-element" width="220" height="163" data-durationhint="4" data-mwtitle="Pulsar_anim.ogv" data-mwprovider="wikimediacommons" resource="/wiki/File:Pulsar_anim.ogv"><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/b/b7/Pulsar_anim.ogv/Pulsar_anim.ogv.480p.vp9.webm" type="video/webm; codecs="vp9, opus"" data-transcodekey="480p.vp9.webm" data-width="648" data-height="480" /><source src="//upload.wikimedia.org/wikipedia/commons/b/b7/Pulsar_anim.ogv" type="video/ogg; codecs="theora"" data-width="800" data-height="592" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/b/b7/Pulsar_anim.ogv/Pulsar_anim.ogv.144p.mjpeg.mov" type="video/quicktime" data-transcodekey="144p.mjpeg.mov" data-width="194" data-height="144" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/b/b7/Pulsar_anim.ogv/Pulsar_anim.ogv.240p.vp9.webm" type="video/webm; codecs="vp9, opus"" data-transcodekey="240p.vp9.webm" data-width="324" data-height="240" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/b/b7/Pulsar_anim.ogv/Pulsar_anim.ogv.360p.webm" type="video/webm; codecs="vp8, vorbis"" data-transcodekey="360p.webm" data-width="486" data-height="360" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/b/b7/Pulsar_anim.ogv/Pulsar_anim.ogv.360p.vp9.webm" type="video/webm; codecs="vp9, opus"" data-transcodekey="360p.vp9.webm" data-width="486" data-height="360" /></video></span><figcaption>Animation of a rotating pulsar. The sphere in the middle represents the neutron star, the curves indicate the magnetic field lines and the protruding cones represent the emission zones.</figcaption></figure> <div class="mw-heading mw-heading3"><h3 id="Pulsars">Pulsars</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=14" title="Edit section: Pulsars"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236090951"><div role="note" class="hatnote navigation-not-searchable">Main article: <a href="/wiki/Pulsar" title="Pulsar">Pulsar</a></div> <p>Neutron stars are detected from their <a href="/wiki/Electromagnetic_radiation" title="Electromagnetic radiation">electromagnetic radiation</a>. Neutron stars are usually observed to <a href="/wiki/Pulse_(physics)" title="Pulse (physics)">pulse</a> <a href="/wiki/Radio_wave" title="Radio wave">radio waves</a> and other electromagnetic radiation, and neutron stars observed with pulses are called pulsars. </p><p>Pulsars' radiation is thought to be caused by particle acceleration near their <a href="/wiki/Poles_of_astronomical_bodies#Magnetic_poles" title="Poles of astronomical bodies">magnetic poles</a>, which need not be aligned with the <a href="/wiki/Axis_of_rotation" class="mw-redirect" title="Axis of rotation">rotational axis</a> of the neutron star. It is thought that a large <a href="/wiki/Electrostatic_field" class="mw-redirect" title="Electrostatic field">electrostatic field</a> builds up near the magnetic poles, leading to <a href="/wiki/Electron_emission" title="Electron emission">electron emission</a>.<sup id="cite_ref-nrao_62-0" class="reference"><a href="#cite_note-nrao-62"><span class="cite-bracket">[</span>59<span class="cite-bracket">]</span></a></sup> These electrons are magnetically accelerated along the field lines, leading to <a href="/wiki/Curvature_radiation" class="mw-redirect" title="Curvature radiation">curvature radiation</a>, with the radiation being strongly <a href="/wiki/Polarization_(waves)" title="Polarization (waves)">polarized</a> towards the plane of curvature.<sup id="cite_ref-nrao_62-1" class="reference"><a href="#cite_note-nrao-62"><span class="cite-bracket">[</span>59<span class="cite-bracket">]</span></a></sup> In addition, high-energy <a href="/wiki/Photons" class="mw-redirect" title="Photons">photons</a> can interact with lower-energy photons and the magnetic field for <a href="/wiki/Electron%E2%88%92positron_pair_production" class="mw-redirect" title="Electron−positron pair production">electron−positron pair production</a>, which through <a href="/wiki/Electron%E2%80%93positron_annihilation" title="Electron–positron annihilation">electron–positron annihilation</a> leads to further high-energy photons.<sup id="cite_ref-nrao_62-2" class="reference"><a href="#cite_note-nrao-62"><span class="cite-bracket">[</span>59<span class="cite-bracket">]</span></a></sup> </p><p>The radiation emanating from the magnetic poles of neutron stars can be described as <i>magnetospheric radiation</i>, in reference to the <a href="/wiki/Magnetosphere" title="Magnetosphere">magnetosphere</a> of the neutron star.<sup id="cite_ref-pavlov_63-0" class="reference"><a href="#cite_note-pavlov-63"><span class="cite-bracket">[</span>60<span class="cite-bracket">]</span></a></sup> It is not to be confused with <i><a href="/wiki/Multipole_radiation" title="Multipole radiation">magnetic dipole radiation</a></i>, which is emitted because the <a href="/wiki/Poles_of_astronomical_bodies#Magnetic_poles" title="Poles of astronomical bodies">magnetic</a> <a href="/wiki/Rotation_around_a_fixed_axis" title="Rotation around a fixed axis">axis</a> is not aligned with the rotational axis, with a radiation frequency the same as the neutron star's rotational frequency.<sup id="cite_ref-nrao_62-3" class="reference"><a href="#cite_note-nrao-62"><span class="cite-bracket">[</span>59<span class="cite-bracket">]</span></a></sup> </p><p>If the axis of rotation of the neutron star is different from the magnetic axis, external viewers will only see these beams of radiation whenever the magnetic axis point towards them during the neutron star rotation. Therefore, <a href="/wiki/Periodic_function" title="Periodic function">periodic</a> pulses are observed, at the same rate as the rotation of the neutron star. </p><p>In May 2022, astronomers reported an ultra-long-period radio-emitting neutron star <a href="/wiki/PSR_J0901-4046" class="mw-redirect" title="PSR J0901-4046">PSR J0901-4046</a>, with spin properties distinct from the known neutron stars.<sup id="cite_ref-64" class="reference"><a href="#cite_note-64"><span class="cite-bracket">[</span>61<span class="cite-bracket">]</span></a></sup> It is unclear how its radio emission is generated, and it challenges the current understanding of how pulsars evolve.<sup id="cite_ref-65" class="reference"><a href="#cite_note-65"><span class="cite-bracket">[</span>62<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading3"><h3 id="Non-pulsating_neutron_stars">Non-pulsating neutron stars</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=15" title="Edit section: Non-pulsating neutron stars"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>In addition to pulsars, non-pulsating neutron stars have also been identified, although they may have minor periodic variation in luminosity.<sup id="cite_ref-cco_66-0" class="reference"><a href="#cite_note-cco-66"><span class="cite-bracket">[</span>63<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-non-pulsating_67-0" class="reference"><a href="#cite_note-non-pulsating-67"><span class="cite-bracket">[</span>64<span class="cite-bracket">]</span></a></sup> This seems to be a characteristic of the X-ray sources known as <a href="/wiki/Central_Compact_Object" class="mw-redirect" title="Central Compact Object">Central Compact Objects</a> in <a href="/wiki/Supernova_remnant" title="Supernova remnant">supernova remnants</a> (CCOs in SNRs), which are thought to be young, radio-quiet isolated neutron stars.<sup id="cite_ref-cco_66-1" class="reference"><a href="#cite_note-cco-66"><span class="cite-bracket">[</span>63<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading3"><h3 id="Spectra">Spectra</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=16" title="Edit section: Spectra"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>In addition to <a href="/wiki/Radio_wave" title="Radio wave">radio</a> emissions, neutron stars have also been identified in other parts of the <a href="/wiki/Electromagnetic_spectrum" title="Electromagnetic spectrum">electromagnetic spectrum</a>. This includes <a href="/wiki/Light" title="Light">visible light</a>, <a href="/wiki/Near_infrared" class="mw-redirect" title="Near infrared">near infrared</a>, <a href="/wiki/Ultraviolet" title="Ultraviolet">ultraviolet</a>, <a href="/wiki/X-ray" title="X-ray">X-rays</a>, and <a href="/wiki/Gamma_ray" title="Gamma ray">gamma rays</a>.<sup id="cite_ref-pavlov_63-1" class="reference"><a href="#cite_note-pavlov-63"><span class="cite-bracket">[</span>60<span class="cite-bracket">]</span></a></sup> Pulsars observed in X-rays are known as <a href="/wiki/Accretion-powered_pulsars" class="mw-redirect" title="Accretion-powered pulsars">X-ray pulsars if accretion-powered</a>, while those identified in visible light are known as <a href="/wiki/Optical_pulsar" title="Optical pulsar">optical pulsars</a>. The majority of neutron stars detected, including those identified in optical, X-ray, and gamma rays, also emit radio waves;<sup id="cite_ref-jb_68-0" class="reference"><a href="#cite_note-jb-68"><span class="cite-bracket">[</span>65<span class="cite-bracket">]</span></a></sup> the <a href="/wiki/Crab_Pulsar" title="Crab Pulsar">Crab Pulsar</a> produces electromagnetic emissions across the spectrum.<sup id="cite_ref-jb_68-1" class="reference"><a href="#cite_note-jb-68"><span class="cite-bracket">[</span>65<span class="cite-bracket">]</span></a></sup> However, there exist neutron stars called <a href="/wiki/Radio-quiet_neutron_star" title="Radio-quiet neutron star">radio-quiet neutron stars</a>, with no radio emissions detected.<sup id="cite_ref-ras_69-0" class="reference"><a href="#cite_note-ras-69"><span class="cite-bracket">[</span>66<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading2"><h2 id="Rotation">Rotation</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=17" title="Edit section: Rotation"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Neutron stars rotate extremely rapidly after their formation due to the conservation of angular momentum; in analogy to spinning ice skaters pulling in their arms, the slow rotation of the original star's core speeds up as it shrinks. A newborn neutron star can rotate many times a second. </p> <div class="mw-heading mw-heading3"><h3 id="Spin_down">Spin down</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=18" title="Edit section: Spin down"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:PPdot2.png" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/b/b9/PPdot2.png/220px-PPdot2.png" decoding="async" width="220" height="154" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/b/b9/PPdot2.png/330px-PPdot2.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/b/b9/PPdot2.png/440px-PPdot2.png 2x" data-file-width="1600" data-file-height="1120" /></a><figcaption><i>P</i>–<i>P</i>-dot diagram for known <a href="/wiki/Rotation-powered_pulsar" class="mw-redirect" title="Rotation-powered pulsar">rotation-powered pulsars</a> (red), anomalous X-ray pulsars (green), high-energy emission pulsars (blue) and <a href="/wiki/Binary_pulsar" title="Binary pulsar">binary pulsars</a> (pink)</figcaption></figure> <p>Over time, neutron stars slow, as their rotating magnetic fields in effect radiate energy associated with the rotation; older neutron stars may take several seconds for each revolution. This is called <i>spin down</i>. The rate at which a neutron star slows its rotation is usually constant and very small. </p><p>The <a href="/wiki/Periodic_time" class="mw-redirect" title="Periodic time">periodic time</a> (<i>P</i>) is the <a href="/wiki/Rotation_period" class="mw-redirect" title="Rotation period">rotational period</a>, the time for one rotation of a neutron star. The spin-down rate, the rate of slowing of rotation, is then given the symbol <span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle {\dot {P}}}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mrow class="MJX-TeXAtom-ORD"> <mrow class="MJX-TeXAtom-ORD"> <mover> <mi>P</mi> <mo>˙</mo> </mover> </mrow> </mrow> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle {\dot {P}}}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/3a125189b1b82db5376a0f97fe2278089972f9be" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.338ex; width:1.812ex; height:2.676ex;" alt="{\displaystyle {\dot {P}}}"></span> (<i>P</i>-dot), the <a href="/wiki/Derivative" title="Derivative">derivative</a> of <i>P</i> with respect to time. It is defined as periodic time increase per unit time; it is a <a href="/wiki/Dimensionless_quantity" title="Dimensionless quantity">dimensionless quantity</a>, but can be given the units of s⋅s<sup>−1</sup> (seconds per second).<sup id="cite_ref-nrao_62-4" class="reference"><a href="#cite_note-nrao-62"><span class="cite-bracket">[</span>59<span class="cite-bracket">]</span></a></sup> </p><p>The spin-down rate (<i>P</i>-dot) of neutron stars usually falls within the range of <span class="nowrap"><span data-sort-value="6978100000000000000♠"></span>10<sup>−22</sup></span> to <span class="nowrap"><span data-sort-value="6991100000000000000♠"></span>10<sup>−9</sup> s⋅s<sup>−1</sup></span>, with the shorter period (or faster rotating) observable neutron stars usually having smaller <i>P</i>-dot. As a neutron star ages, its rotation slows (as <i>P</i> increases); eventually, the rate of rotation will become too slow to power the radio-emission mechanism, so radio emission from the neutron star no longer can be detected.<sup id="cite_ref-nrao_62-5" class="reference"><a href="#cite_note-nrao-62"><span class="cite-bracket">[</span>59<span class="cite-bracket">]</span></a></sup> </p><p><i>P</i> and <i>P</i>-dot allow minimum magnetic fields of neutron stars to be estimated.<sup id="cite_ref-nrao_62-6" class="reference"><a href="#cite_note-nrao-62"><span class="cite-bracket">[</span>59<span class="cite-bracket">]</span></a></sup> <i>P</i> and <i>P</i>-dot can be also used to calculate the <i>characteristic age</i> of a pulsar, but gives an estimate which is somewhat larger than the true age when it is applied to young pulsars.<sup id="cite_ref-nrao_62-7" class="reference"><a href="#cite_note-nrao-62"><span class="cite-bracket">[</span>59<span class="cite-bracket">]</span></a></sup> </p><p><i>P</i> and <i>P</i>-dot can also be combined with neutron star's <a href="/wiki/Moment_of_inertia" title="Moment of inertia">moment of inertia</a> to estimate a quantity called <i>spin-down <a href="/wiki/Luminosity" title="Luminosity">luminosity</a></i>, which is given the symbol <span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle {\dot {E}}}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mrow class="MJX-TeXAtom-ORD"> <mrow class="MJX-TeXAtom-ORD"> <mover> <mi>E</mi> <mo>˙</mo> </mover> </mrow> </mrow> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle {\dot {E}}}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/fc7c4671135d5bd8f253771d9d11b58034287c73" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.338ex; width:1.776ex; height:2.676ex;" alt="{\displaystyle {\dot {E}}}"></span> (<i>E</i>-dot). It is not the measured luminosity, but rather the calculated loss rate of rotational energy that would manifest itself as radiation. For neutron stars where the spin-down luminosity is comparable to the actual <a href="/wiki/Luminosity" title="Luminosity">luminosity</a>, the neutron stars are said to be "<a href="/wiki/Rotation_powered_pulsar" class="mw-redirect" title="Rotation powered pulsar">rotation powered</a>".<sup id="cite_ref-nrao_62-8" class="reference"><a href="#cite_note-nrao-62"><span class="cite-bracket">[</span>59<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-pavlov_63-2" class="reference"><a href="#cite_note-pavlov-63"><span class="cite-bracket">[</span>60<span class="cite-bracket">]</span></a></sup> The observed luminosity of the <a href="/wiki/Crab_Pulsar" title="Crab Pulsar">Crab Pulsar</a> is comparable to the spin-down luminosity, supporting the model that rotational kinetic energy powers the radiation from it.<sup id="cite_ref-nrao_62-9" class="reference"><a href="#cite_note-nrao-62"><span class="cite-bracket">[</span>59<span class="cite-bracket">]</span></a></sup> With neutron stars such as magnetars, where the actual luminosity exceeds the spin-down luminosity by about a factor of one hundred, it is assumed that the luminosity is powered by magnetic dissipation, rather than being rotation powered.<sup id="cite_ref-ufrgs_70-0" class="reference"><a href="#cite_note-ufrgs-70"><span class="cite-bracket">[</span>67<span class="cite-bracket">]</span></a></sup> </p><p><i>P</i> and <i>P</i>-dot can also be plotted for neutron stars to create a <i>P</i>–<i>P</i>-dot diagram. It encodes a tremendous amount of information about the pulsar population and its properties, and has been likened to the <a href="/wiki/Hertzsprung%E2%80%93Russell_diagram" title="Hertzsprung–Russell diagram">Hertzsprung–Russell diagram</a> in its importance for neutron stars.<sup id="cite_ref-nrao_62-10" class="reference"><a href="#cite_note-nrao-62"><span class="cite-bracket">[</span>59<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading3"><h3 id="Spin_up">Spin up</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=19" title="Edit section: Spin up"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Neutron_Star_X-ray_beaming_with_accretion_disk.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/2/23/Neutron_Star_X-ray_beaming_with_accretion_disk.jpg/220px-Neutron_Star_X-ray_beaming_with_accretion_disk.jpg" decoding="async" width="220" height="124" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/2/23/Neutron_Star_X-ray_beaming_with_accretion_disk.jpg/330px-Neutron_Star_X-ray_beaming_with_accretion_disk.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/2/23/Neutron_Star_X-ray_beaming_with_accretion_disk.jpg/440px-Neutron_Star_X-ray_beaming_with_accretion_disk.jpg 2x" data-file-width="3000" data-file-height="1688" /></a><figcaption>A computer simulation depicting a neutron star with accretion disk, spewing out X-rays through the magnetic axis</figcaption></figure> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236090951"><div role="note" class="hatnote navigation-not-searchable">Main article: <a href="/wiki/Neutron_star_spin-up" title="Neutron star spin-up">Neutron star spin-up</a></div> <p>Neutron star rotational speeds can increase, a process known as spin up. Sometimes neutron stars absorb orbiting matter from companion stars, increasing the rotation rate and reshaping the neutron star into an <a href="/wiki/Oblate_spheroid" class="mw-redirect" title="Oblate spheroid">oblate spheroid</a>. This causes an increase in the rate of rotation of the neutron star of over a hundred times per second in the case of millisecond pulsars. </p><p>The most rapidly rotating neutron star currently known, <a href="/wiki/PSR_J1748-2446ad" class="mw-redirect" title="PSR J1748-2446ad">PSR J1748-2446ad</a>, rotates at 716 revolutions per second.<sup id="cite_ref-71" class="reference"><a href="#cite_note-71"><span class="cite-bracket">[</span>68<span class="cite-bracket">]</span></a></sup> A 2007 paper reported the detection of an X-ray burst oscillation, which provides an indirect measure of spin, of 1122 <a href="/wiki/Hertz" title="Hertz">Hz</a> from the neutron star <a href="/wiki/XTE_J1739-285" title="XTE J1739-285">XTE J1739-285</a>,<sup id="cite_ref-KaaretPrieskorn2007_72-0" class="reference"><a href="#cite_note-KaaretPrieskorn2007-72"><span class="cite-bracket">[</span>69<span class="cite-bracket">]</span></a></sup> suggesting 1122 rotations a second. However, at present, this signal has only been seen once, and should be regarded as tentative until confirmed in another burst from that star. </p> <div class="mw-heading mw-heading3"><h3 id="Glitches_and_starquakes">Glitches and starquakes</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=20" title="Edit section: Glitches and starquakes"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:2004_stellar_quake_full.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/e/ed/2004_stellar_quake_full.jpg/220px-2004_stellar_quake_full.jpg" decoding="async" width="220" height="172" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/e/ed/2004_stellar_quake_full.jpg/330px-2004_stellar_quake_full.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/e/ed/2004_stellar_quake_full.jpg/440px-2004_stellar_quake_full.jpg 2x" data-file-width="3868" data-file-height="3024" /></a><figcaption>NASA artist's conception of a "<a href="/wiki/Starquake_(astrophysics)#Starquake" class="mw-redirect" title="Starquake (astrophysics)">starquake</a>", or "stellar quake"</figcaption></figure> <p>Sometimes a neutron star will undergo a <a href="/wiki/Glitch_(astronomy)" title="Glitch (astronomy)">glitch</a>, a sudden small increase of its rotational speed or spin up.<sup id="cite_ref-:0_73-0" class="reference"><a href="#cite_note-:0-73"><span class="cite-bracket">[</span>70<span class="cite-bracket">]</span></a></sup> Glitches are thought to be the effect of a <a href="/wiki/Starquake_(astrophysics)" class="mw-redirect" title="Starquake (astrophysics)">starquake</a>—as the rotation of the neutron star slows, its shape becomes more spherical. Due to the stiffness of the "neutron" crust, this happens as discrete events when the crust ruptures, creating a starquake similar to earthquakes. After the starquake, the star will have a smaller equatorial radius, and because angular momentum is conserved, its rotational speed has increased. </p><p>Starquakes occurring in <a href="/wiki/Magnetars" class="mw-redirect" title="Magnetars">magnetars</a>, with a resulting glitch, is the leading hypothesis for the gamma-ray sources known as soft gamma repeaters.<sup id="cite_ref-sa_44-1" class="reference"><a href="#cite_note-sa-44"><span class="cite-bracket">[</span>42<span class="cite-bracket">]</span></a></sup> </p><p>Recent work, however, suggests that a starquake would not release sufficient energy for a neutron star glitch; it has been suggested that glitches may instead be caused by transitions of vortices in the theoretical superfluid core of the neutron star from one metastable energy state to a lower one, thereby releasing energy that appears as an increase in the rotation rate.<sup id="cite_ref-74" class="reference"><a href="#cite_note-74"><span class="cite-bracket">[</span>71<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-:0_73-1" class="reference"><a href="#cite_note-:0-73"><span class="cite-bracket">[</span>70<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading3"><h3 id="Anti-glitches">Anti-glitches</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=21" title="Edit section: Anti-glitches"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>An anti-glitch, a sudden small decrease in rotational speed, or spin down, of a neutron star has also been reported.<sup id="cite_ref-nature_75-0" class="reference"><a href="#cite_note-nature-75"><span class="cite-bracket">[</span>72<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-76" class="reference"><a href="#cite_note-76"><span class="cite-bracket">[</span>73<span class="cite-bracket">]</span></a></sup> It occurred in the magnetar <a href="/w/index.php?title=1E_2259%2B586&action=edit&redlink=1" class="new" title="1E 2259+586 (page does not exist)">1E 2259+586</a>, that in one case produced an X-ray luminosity increase of a factor of 20, and a significant spin-down rate change. Current neutron star models do not predict this behavior. If the cause were internal this suggests differential rotation of the solid outer crust and the superfluid component of the magnetar's inner structure.<sup id="cite_ref-nature_75-1" class="reference"><a href="#cite_note-nature-75"><span class="cite-bracket">[</span>72<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-:0_73-2" class="reference"><a href="#cite_note-:0-73"><span class="cite-bracket">[</span>70<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading2"><h2 id="Population_and_distances">Population and distances</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=22" title="Edit section: Population and distances"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>At present, there are about 3,200 known neutron stars in the <a href="/wiki/Milky_Way" title="Milky Way">Milky Way</a> and the <a href="/wiki/Magellanic_Clouds" title="Magellanic Clouds">Magellanic Clouds</a>, the majority of which have been detected as radio pulsars. Neutron stars are mostly concentrated along the disk of the Milky Way, although the spread perpendicular to the disk is large because the supernova explosion process can impart high translational speeds (400 km/s) to the newly formed neutron star. </p><p>Some of the closest known neutron stars are RX J1856.5−3754, which is about 400 <a href="/wiki/Light-year" title="Light-year">light-years</a> from Earth, and <a href="/wiki/PSR_J0108%E2%88%921431" title="PSR J0108−1431">PSR J0108−1431</a> about 424 light-years.<sup id="cite_ref-aaa496_77-0" class="reference"><a href="#cite_note-aaa496-77"><span class="cite-bracket">[</span>74<span class="cite-bracket">]</span></a></sup> RX J1856.5-3754 is a member of a close group of neutron stars called <a href="/wiki/The_Magnificent_Seven_(neutron_stars)" title="The Magnificent Seven (neutron stars)">The Magnificent Seven</a>. Another nearby neutron star that was detected transiting the backdrop of the constellation Ursa Minor has been nicknamed <a href="/wiki/Calvera_(X-ray_source)" title="Calvera (X-ray source)">Calvera</a> by its Canadian and American discoverers, after the villain in the 1960 film <i><a href="/wiki/The_Magnificent_Seven" title="The Magnificent Seven">The Magnificent Seven</a></i>. This rapidly moving object was discovered using the <a href="/wiki/ROSAT" title="ROSAT">ROSAT</a> Bright Source Catalog. </p><p>Neutron stars are only detectable with modern technology during the earliest stages of their lives (almost always less than 1 million years) and are vastly outnumbered by older neutron stars that would only be detectable through their <a href="/wiki/Black-body_radiation" title="Black-body radiation">blackbody radiation</a> and gravitational effects on other stars. </p> <div class="mw-heading mw-heading2"><h2 id="Binary_neutron_star_systems">Binary neutron star systems</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=23" title="Edit section: Binary neutron star systems"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p><span class="anchor" id="Binary_neutron_stars"></span> </p> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:15-137-CircinusX1-XRayLightRings-NeutronStar-Chandra-20150624.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/6/60/15-137-CircinusX1-XRayLightRings-NeutronStar-Chandra-20150624.jpg/220px-15-137-CircinusX1-XRayLightRings-NeutronStar-Chandra-20150624.jpg" decoding="async" width="220" height="220" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/6/60/15-137-CircinusX1-XRayLightRings-NeutronStar-Chandra-20150624.jpg/330px-15-137-CircinusX1-XRayLightRings-NeutronStar-Chandra-20150624.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/6/60/15-137-CircinusX1-XRayLightRings-NeutronStar-Chandra-20150624.jpg/440px-15-137-CircinusX1-XRayLightRings-NeutronStar-Chandra-20150624.jpg 2x" data-file-width="3600" data-file-height="3600" /></a><figcaption><a href="/wiki/Circinus_X-1" title="Circinus X-1">Circinus X-1</a>: X-ray light rings from a binary neutron star (24 June 2015; <a href="/wiki/Chandra_X-ray_Observatory" title="Chandra X-ray Observatory">Chandra X-ray Observatory</a>)</figcaption></figure> <p>About 5% of all known neutron stars are members of a <a href="/wiki/Binary_system_(astronomy)" class="mw-redirect" title="Binary system (astronomy)">binary system</a>. The formation and evolution of binary neutron stars<sup id="cite_ref-78" class="reference"><a href="#cite_note-78"><span class="cite-bracket">[</span>75<span class="cite-bracket">]</span></a></sup> and double neutron stars<sup id="cite_ref-TaurisKramerFreire2017_79-0" class="reference"><a href="#cite_note-TaurisKramerFreire2017-79"><span class="cite-bracket">[</span>76<span class="cite-bracket">]</span></a></sup> can be a complex process. Neutron stars have been observed in binaries with ordinary <a href="/wiki/Main-sequence_star" class="mw-redirect" title="Main-sequence star">main-sequence stars</a>, <a href="/wiki/Red_giant" title="Red giant">red giants</a>, white dwarfs, or other neutron stars. According to modern theories of binary evolution, it is expected that neutron stars also exist in binary systems with black hole companions. The merger of binaries containing two neutron stars, or a neutron star and a black hole, has been observed through the emission of <a href="/wiki/Gravitational_waves" class="mw-redirect" title="Gravitational waves">gravitational waves</a>.<sup id="cite_ref-80" class="reference"><a href="#cite_note-80"><span class="cite-bracket">[</span>77<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-81" class="reference"><a href="#cite_note-81"><span class="cite-bracket">[</span>78<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading3"><h3 id="X-ray_binaries">X-ray binaries</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=24" title="Edit section: X-ray binaries"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236090951"><div role="note" class="hatnote navigation-not-searchable">Main article: <a href="/wiki/X-ray_binary" title="X-ray binary">X-ray binary</a></div> <p>Binary systems containing neutron stars often emit X-rays, which are emitted by hot gas as it falls towards the surface of the neutron star. The source of the gas is the companion star, the outer layers of which can be stripped off by the gravitational force of the neutron star if the two stars are sufficiently close. As the neutron star accretes this gas, its mass can increase; if enough mass is accreted, the neutron star may collapse into a black hole.<sup id="cite_ref-lewin2010_82-0" class="reference"><a href="#cite_note-lewin2010-82"><span class="cite-bracket">[</span>79<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading3"><h3 id="Neutron_star_binary_mergers_and_nucleosynthesis">Neutron star binary mergers and nucleosynthesis</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=25" title="Edit section: Neutron star binary mergers and nucleosynthesis"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236090951"><div role="note" class="hatnote navigation-not-searchable">Main article: <a href="/wiki/Neutron_star_merger" title="Neutron star merger">Neutron star merger</a></div> 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href="/wiki/File:Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_(GSFC_20171208_Archive_e001098).jpg" class="mw-file-description"><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/b/ba/Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001098%29.jpg/142px-Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001098%29.jpg" decoding="async" width="142" height="114" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/b/ba/Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001098%29.jpg/213px-Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001098%29.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/b/ba/Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001098%29.jpg/284px-Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001098%29.jpg 2x" data-file-width="4000" data-file-height="3200" /></a></span></div></div><div class="tsingle" style="width:144px;max-width:144px"><div class="thumbimage" style="height:113px;overflow:hidden"><span typeof="mw:File"><a href="/wiki/File:Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_(GSFC_20171208_Archive_e001099).jpg" class="mw-file-description"><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/a/a9/Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001099%29.jpg/142px-Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001099%29.jpg" decoding="async" width="142" height="114" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/a/a9/Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001099%29.jpg/213px-Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001099%29.jpg 1.5x, 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srcset="//upload.wikimedia.org/wikipedia/commons/thumb/8/84/Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001100%29.jpg/176px-Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001100%29.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/8/84/Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001100%29.jpg/234px-Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001100%29.jpg 2x" data-file-width="4000" data-file-height="3200" /></a></span></div></div><div class="tsingle" style="width:169px;max-width:169px"><div class="thumbimage" style="height:93px;overflow:hidden"><span typeof="mw:File"><a href="/wiki/File:Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_(GSFC_20171208_Archive_e001101).jpg" class="mw-file-description"><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/6/62/Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001101%29.jpg/167px-Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001101%29.jpg" decoding="async" width="167" height="94" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/6/62/Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001101%29.jpg/251px-Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001101%29.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/6/62/Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001101%29.jpg/334px-Neutron_Stars_Rip_Each_Other_Apart_to_Form_Black_Hole_%28GSFC_20171208_Archive_e001101%29.jpg 2x" data-file-width="1920" data-file-height="1080" /></a></span></div></div></div><div class="trow" style="display:flex"><div class="thumbcaption">Four snapshots from a computer simulation of a neutron star merger. Clockwise, from top left: <ol><li>The two neutron stars make initial contact</li> <li>Immense tidal forces begin to disrupt the outer layers of the neutron stars</li> <li>The neutron stars are completely tidally disrupted</li> <li>A black hole forms, surrounded by an accretion disc</li></ol></div></div></div></div> <p>The distance between two neutron stars in a close binary system is observed to shrink as <a href="/wiki/Gravitational_waves" class="mw-redirect" title="Gravitational waves">gravitational waves</a> are emitted.<sup id="cite_ref-83" class="reference"><a href="#cite_note-83"><span class="cite-bracket">[</span>80<span class="cite-bracket">]</span></a></sup> Ultimately, the neutron stars will come into contact and coalesce. The coalescence of binary neutron stars is one of the leading models for the origin of <a href="/wiki/Gamma-ray_burst#Short_gamma-ray_bursts" title="Gamma-ray burst">short gamma-ray bursts</a>. Strong evidence for this model came from the observation of a <a href="/wiki/Kilonova" title="Kilonova">kilonova</a> associated with the short-duration gamma-ray burst GRB 130603B,<sup id="cite_ref-84" class="reference"><a href="#cite_note-84"><span class="cite-bracket">[</span>81<span class="cite-bracket">]</span></a></sup> and was finally confirmed by detection of gravitational wave <a href="/wiki/GW170817" title="GW170817">GW170817</a> and short <a href="/wiki/GRB_170817A" class="mw-redirect" title="GRB 170817A">GRB 170817A</a> by <a href="/wiki/LIGO" title="LIGO">LIGO</a>, <a href="/wiki/Virgo_interferometer" title="Virgo interferometer">Virgo</a>, and 70 observatories covering the electromagnetic spectrum observing the event.<sup id="cite_ref-SM-20171016_85-0" class="reference"><a href="#cite_note-SM-20171016-85"><span class="cite-bracket">[</span>82<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-NYT-20171016_86-0" class="reference"><a href="#cite_note-NYT-20171016-86"><span class="cite-bracket">[</span>83<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-NAT-20170825_87-0" class="reference"><a href="#cite_note-NAT-20170825-87"><span class="cite-bracket">[</span>84<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-PhysRev_88-0" class="reference"><a href="#cite_note-PhysRev-88"><span class="cite-bracket">[</span>85<span class="cite-bracket">]</span></a></sup> The light emitted in the kilonova is believed to come from the radioactive decay of material ejected in the merger of the two neutron stars. The merger momentarily creates an environment of such extreme neutron flux that the <a href="/wiki/R-process" title="R-process"><i>r</i>-process</a> can occur; this—as opposed to <a href="/wiki/Supernova_nucleosynthesis" title="Supernova nucleosynthesis">supernova nucleosynthesis</a>—may be responsible for the production of around half the isotopes in <a href="/wiki/Chemical_element" title="Chemical element">chemical elements</a> beyond <a href="/wiki/Iron" title="Iron">iron</a>.<sup id="cite_ref-89" class="reference"><a href="#cite_note-89"><span class="cite-bracket">[</span>86<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading2"><h2 id="Planets">Planets</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=26" title="Edit section: Planets"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236090951"><div role="note" class="hatnote navigation-not-searchable">Main articles: <a href="/wiki/Pulsar_planet" title="Pulsar planet">Pulsar planet</a> and <a href="/wiki/Habitability_of_neutron_star_systems" title="Habitability of neutron star systems">Habitability of neutron star systems</a></div> <p>Neutron stars can host <a href="/wiki/Exoplanet" title="Exoplanet">exoplanets</a>. These can be original, <a href="/wiki/Circumbinary_planet" title="Circumbinary planet">circumbinary</a>, captured, or the result of a second round of planet formation. Pulsars can also strip the atmosphere off from a star, leaving a planetary-mass remnant, which may be understood as a <a href="/wiki/Chthonian_planet" title="Chthonian planet">chthonian planet</a> or a stellar object depending on interpretation. For pulsars, such <a href="/wiki/Pulsar_planet" title="Pulsar planet">pulsar planets</a> can be detected with the <a href="/wiki/Pulsar_timing_method" class="mw-redirect" title="Pulsar timing method">pulsar timing method</a>, which allows for high precision and detection of much smaller planets than with other methods. Two systems have been definitively confirmed. The first exoplanets ever to be detected were the three planets <a href="/wiki/PSR_B1257%2B12_A" title="PSR B1257+12 A">Draugr</a>, <a href="/wiki/PSR_B1257%2B12_B" title="PSR B1257+12 B">Poltergeist</a> and <a href="/wiki/PSR_B1257%2B12_C" title="PSR B1257+12 C">Phobetor</a> around the pulsar <a href="/wiki/PSR_B1257%2B12" title="PSR B1257+12">Lich</a>, discovered in 1992–1994. Of these, Draugr is the smallest exoplanet ever detected, at a mass of twice that of the Moon. Another system is <a href="/wiki/PSR_B1620%E2%88%9226" title="PSR B1620−26">PSR B1620−26</a>, where a <a href="/wiki/Circumbinary_planet" title="Circumbinary planet">circumbinary planet</a> orbits a neutron star-white dwarf binary system. Also, there are several unconfirmed candidates. Pulsar planets receive little visible light, but massive amounts of ionizing radiation and high-energy stellar wind, which makes them rather hostile environments to life as presently understood. </p> <div class="mw-heading mw-heading2"><h2 id="History_of_discoveries">History of discoveries</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=27" title="Edit section: History of discoveries"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size mw-halign-left" typeof="mw:File/Thumb"><a href="/wiki/File:Isolated_Neutron_Star_RX_J185635-3754_-_opo9732a.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/3/33/Isolated_Neutron_Star_RX_J185635-3754_-_opo9732a.jpg/220px-Isolated_Neutron_Star_RX_J185635-3754_-_opo9732a.jpg" decoding="async" width="220" height="275" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/3/33/Isolated_Neutron_Star_RX_J185635-3754_-_opo9732a.jpg/330px-Isolated_Neutron_Star_RX_J185635-3754_-_opo9732a.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/3/33/Isolated_Neutron_Star_RX_J185635-3754_-_opo9732a.jpg/440px-Isolated_Neutron_Star_RX_J185635-3754_-_opo9732a.jpg 2x" data-file-width="2400" data-file-height="3000" /></a><figcaption>The first direct observation of an isolated neutron star in visible light. The neutron star is RX J1856.5−3754.</figcaption></figure> <p>At the meeting of the <a href="/wiki/American_Physical_Society" title="American Physical Society">American Physical Society</a> in December 1933 (the proceedings were published in January 1934), <a href="/wiki/Walter_Baade" title="Walter Baade">Walter Baade</a> and <a href="/wiki/Fritz_Zwicky" title="Fritz Zwicky">Fritz Zwicky</a> proposed the existence of neutron stars,<sup id="cite_ref-90" class="reference"><a href="#cite_note-90"><span class="cite-bracket">[</span>87<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-93" class="reference"><a href="#cite_note-93"><span class="cite-bracket">[</span>d<span class="cite-bracket">]</span></a></sup> less than two years after <a href="/wiki/Discovery_of_the_neutron" title="Discovery of the neutron">the discovery of the neutron</a> by <a href="/wiki/James_Chadwick" title="James Chadwick">James Chadwick</a>.<sup id="cite_ref-94" class="reference"><a href="#cite_note-94"><span class="cite-bracket">[</span>90<span class="cite-bracket">]</span></a></sup> In seeking an explanation for the origin of a <a href="/wiki/Supernova" title="Supernova">supernova</a>, they tentatively proposed that in supernova explosions ordinary stars are turned into stars that consist of extremely closely packed neutrons that they called neutron stars. Baade and Zwicky correctly proposed at that time that the release of the gravitational binding energy of the neutron stars powers the supernova: "In the supernova process, mass in bulk is annihilated". Neutron stars were thought to be too faint to be detectable and little work was done on them until November 1967, when <a href="/wiki/Franco_Pacini" title="Franco Pacini">Franco Pacini</a> pointed out that if the neutron stars were spinning and had large magnetic fields, then electromagnetic waves would be emitted. Unknown to him, radio astronomer <a href="/wiki/Antony_Hewish" title="Antony Hewish">Antony Hewish</a> and his graduate student <a href="/wiki/Jocelyn_Bell" class="mw-redirect" title="Jocelyn Bell">Jocelyn Bell</a> at Cambridge were shortly to detect radio pulses from stars that are now believed to be highly magnetized, rapidly spinning neutron stars, known as pulsars. </p><p>In 1965, Antony Hewish and <a href="/wiki/Samuel_Okoye" title="Samuel Okoye">Samuel Okoye</a> discovered "an unusual source of high radio brightness temperature in the <a href="/wiki/Crab_Nebula" title="Crab Nebula">Crab Nebula</a>".<sup id="cite_ref-95" class="reference"><a href="#cite_note-95"><span class="cite-bracket">[</span>91<span class="cite-bracket">]</span></a></sup> This source turned out to be the Crab Pulsar that resulted from the great <a href="/wiki/SN_1054" title="SN 1054">supernova of 1054</a>. </p><p>In 1967, <a href="/wiki/Iosif_Shklovsky" title="Iosif Shklovsky">Iosif Shklovsky</a> examined the X-ray and optical observations of <a href="/wiki/Scorpius_X-1" title="Scorpius X-1">Scorpius X-1</a> and correctly concluded that the radiation comes from a neutron star at the stage of <a href="/wiki/Accretion_(astrophysics)" title="Accretion (astrophysics)">accretion</a>.<sup id="cite_ref-96" class="reference"><a href="#cite_note-96"><span class="cite-bracket">[</span>92<span class="cite-bracket">]</span></a></sup> </p><p>In 1967, Jocelyn Bell Burnell and Antony Hewish discovered regular radio pulses from <a href="/wiki/PSR_B1919%2B21" title="PSR B1919+21">PSR B1919+21</a>. This pulsar was later interpreted as an isolated, rotating neutron star. The energy source of the pulsar is the rotational energy of the neutron star. The majority of known neutron stars (about 2000, as of 2010) have been discovered as pulsars, emitting regular radio pulses. </p><p>In 1968, <a href="/wiki/Richard_V._E._Lovelace" title="Richard V. E. Lovelace">Richard V. E. Lovelace</a> and collaborators discovered period <span class="mwe-math-element"><span class="mwe-math-mathml-inline mwe-math-mathml-a11y" style="display: none;"><math xmlns="http://www.w3.org/1998/Math/MathML" alttext="{\displaystyle P\!\approx 33}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>P</mi> <mspace width="negativethinmathspace" /> <mo>≈</mo> <mn>33</mn> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle P\!\approx 33}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/6928f373cf1be6a939109ffba363b0fcdb8fa447" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.338ex; width:6.782ex; height:2.176ex;" alt="{\displaystyle P\!\approx 33}"></span> ms of the <a href="/wiki/Crab_pulsar" class="mw-redirect" title="Crab pulsar">Crab pulsar</a> using <a href="/wiki/Arecibo_Observatory" title="Arecibo Observatory">Arecibo Observatory</a>.<sup id="cite_ref-Lovelace1969_97-0" class="reference"><a href="#cite_note-Lovelace1969-97"><span class="cite-bracket">[</span>93<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-Lovelace1969a_98-0" class="reference"><a href="#cite_note-Lovelace1969a-98"><span class="cite-bracket">[</span>94<span class="cite-bracket">]</span></a></sup> After this discovery, scientists concluded that <a href="/wiki/Pulsars" class="mw-redirect" title="Pulsars">pulsars</a> were rotating <a href="/wiki/Neutron_stars" class="mw-redirect" title="Neutron stars">neutron stars</a>.<sup id="cite_ref-LovelaceTyler2012_99-0" class="reference"><a href="#cite_note-LovelaceTyler2012-99"><span class="cite-bracket">[</span>95<span class="cite-bracket">]</span></a></sup> Before that, many scientists believed that pulsars were pulsating <a href="/wiki/White_dwarfs" class="mw-redirect" title="White dwarfs">white dwarfs</a>. </p><p>In 1971, <a href="/wiki/Riccardo_Giacconi" title="Riccardo Giacconi">Riccardo Giacconi</a>, Herbert Gursky, Ed Kellogg, R. Levinson, E. Schreier, and H. Tananbaum discovered 4.8 second pulsations in an X-ray source in the <a href="/wiki/Constellation" title="Constellation">constellation</a> <a href="/wiki/Centaurus" title="Centaurus">Centaurus</a>, <a href="/wiki/Centaurus_X-3" title="Centaurus X-3">Cen X-3</a>.<sup id="cite_ref-100" class="reference"><a href="#cite_note-100"><span class="cite-bracket">[</span>96<span class="cite-bracket">]</span></a></sup> They interpreted this as resulting from a rotating hot neutron star. The energy source is gravitational and results from a <a href="/wiki/Accretion_(astrophysics)" title="Accretion (astrophysics)">rain of gas falling</a> onto the surface of the <a href="/wiki/Accretion-powered_pulsar" class="mw-redirect" title="Accretion-powered pulsar">neutron star</a> from a <a href="/wiki/Companion_star" class="mw-redirect" title="Companion star">companion star</a> or the <a href="/wiki/Interstellar_medium" title="Interstellar medium">interstellar medium</a>. </p><p>In 1974, <a href="/wiki/Antony_Hewish" title="Antony Hewish">Antony Hewish</a> was awarded the <a href="/wiki/Nobel_Prize_in_Physics" title="Nobel Prize in Physics">Nobel Prize in Physics</a> "for his decisive role in the discovery of pulsars" without <a href="/wiki/Jocelyn_Bell" class="mw-redirect" title="Jocelyn Bell">Jocelyn Bell</a> who shared in the discovery.<sup id="cite_ref-101" class="reference"><a href="#cite_note-101"><span class="cite-bracket">[</span>97<span class="cite-bracket">]</span></a></sup> </p><p>In 1974, <a href="/wiki/Joseph_Hooton_Taylor_Jr." title="Joseph Hooton Taylor Jr.">Joseph Taylor</a> and <a href="/wiki/Russell_Hulse" class="mw-redirect" title="Russell Hulse">Russell Hulse</a> discovered the first binary pulsar, <a href="/wiki/PSR_B1913%2B16" class="mw-redirect" title="PSR B1913+16">PSR B1913+16</a>, which consists of two neutron stars (one seen as a pulsar) orbiting around their center of mass. <a href="/wiki/Albert_Einstein" title="Albert Einstein">Albert Einstein</a>'s <a href="/wiki/General_relativity" title="General relativity">general theory of relativity</a> predicts that massive objects in short binary orbits should emit <a href="/wiki/Gravitational_wave" title="Gravitational wave">gravitational waves</a>, and thus that their orbit should decay with time. This was indeed observed, precisely as general relativity predicts, and in 1993, Taylor and Hulse were awarded the <a href="/wiki/Nobel_Prize_in_Physics" title="Nobel Prize in Physics">Nobel Prize in Physics</a> for this discovery.<sup id="cite_ref-102" class="reference"><a href="#cite_note-102"><span class="cite-bracket">[</span>98<span class="cite-bracket">]</span></a></sup> </p><p>In 1982, <a href="/wiki/Don_Backer" class="mw-redirect" title="Don Backer">Don Backer</a> and colleagues discovered the first millisecond pulsar, <a href="/wiki/PSR_B1937%2B21" title="PSR B1937+21">PSR B1937+21</a>.<sup id="cite_ref-103" class="reference"><a href="#cite_note-103"><span class="cite-bracket">[</span>99<span class="cite-bracket">]</span></a></sup> This object spins 642 times per second, a value that placed fundamental constraints on the mass and radius of neutron stars. Many millisecond pulsars were later discovered, but PSR B1937+21 remained the fastest-spinning known pulsar for 24 years, until <a href="/wiki/PSR_J1748-2446ad" class="mw-redirect" title="PSR J1748-2446ad">PSR J1748-2446ad</a> (which spins ~716 times a second) was discovered. </p><p>In 2003, <a href="/wiki/Marta_Burgay" title="Marta Burgay">Marta Burgay</a> and colleagues discovered the first double neutron star system where both components are detectable as pulsars, <a href="/wiki/PSR_J0737%E2%88%923039" title="PSR J0737−3039">PSR J0737−3039</a>.<sup id="cite_ref-104" class="reference"><a href="#cite_note-104"><span class="cite-bracket">[</span>100<span class="cite-bracket">]</span></a></sup> The discovery of this system allows a total of 5 different tests of general relativity, some of these with unprecedented precision. </p><p>In 2010, Paul Demorest and colleagues measured the mass of the millisecond pulsar <a href="/wiki/PSR_J1614%E2%88%922230" title="PSR J1614−2230">PSR J1614−2230</a> to be <span class="nowrap"><span data-sort-value="7000197000000000000♠"></span>1.97<span style="margin-left:0.3em;margin-right:0.15em;">±</span>0.04</span> <var>M</var><sub>☉</sub>, using <a href="/wiki/Shapiro_delay" class="mw-redirect" title="Shapiro delay">Shapiro delay</a>.<sup id="cite_ref-105" class="reference"><a href="#cite_note-105"><span class="cite-bracket">[</span>101<span class="cite-bracket">]</span></a></sup> This was substantially higher than any previously measured neutron star mass (1.67 <var>M</var><sub>☉</sub>, see <a href="/wiki/PSR_J1903%2B0327" title="PSR J1903+0327">PSR J1903+0327</a>), and places strong constraints on the interior composition of neutron stars. </p><p>In 2013, <a href="/wiki/John_Antoniadis" title="John Antoniadis">John Antoniadis</a> and colleagues measured the mass of <a href="/wiki/PSR_J0348%2B0432" title="PSR J0348+0432">PSR J0348+0432</a> to be <span class="nowrap"><span data-sort-value="7000200999999999999♠"></span>2.01<span style="margin-left:0.3em;margin-right:0.15em;">±</span>0.04</span> <var>M</var><sub>☉</sub>, using white dwarf spectroscopy.<sup id="cite_ref-106" class="reference"><a href="#cite_note-106"><span class="cite-bracket">[</span>102<span class="cite-bracket">]</span></a></sup> This confirmed the existence of such massive stars using a different method. Furthermore, this allowed, for the first time, a test of <a href="/wiki/General_relativity" title="General relativity">general relativity</a> using such a massive neutron star. </p><p>In August 2017, LIGO and Virgo made first detection of gravitational waves produced by colliding neutron stars (<a href="/wiki/GW170817" title="GW170817">GW170817</a>),<sup id="cite_ref-107" class="reference"><a href="#cite_note-107"><span class="cite-bracket">[</span>103<span class="cite-bracket">]</span></a></sup> leading to further discoveries about neutron stars. </p><p>In October 2018, astronomers reported that <a href="/wiki/GRB_150101B" title="GRB 150101B">GRB 150101B</a>, a <a href="/wiki/Gamma-ray_burst" title="Gamma-ray burst">gamma-ray burst</a> event detected in 2015, may be directly related to the historic GW170817 and associated with the <a href="/wiki/Neutron_star_merger" title="Neutron star merger">merger of two neutron stars</a>. The similarities between the two events, in terms of <a href="/wiki/Gamma_ray" title="Gamma ray">gamma ray</a>, <a href="/wiki/Optical" class="mw-redirect" title="Optical">optical</a> and x-ray emissions, as well as to the nature of the associated host <a href="/wiki/Galaxy" title="Galaxy">galaxies</a>, are "striking", suggesting the two separate events may both be the result of the merger of neutron stars, and both may be a <a href="/wiki/Kilonova" title="Kilonova">kilonova</a>, which may be more common in the universe than previously understood, according to the researchers.<sup id="cite_ref-EA-20181016_108-0" class="reference"><a href="#cite_note-EA-20181016-108"><span class="cite-bracket">[</span>104<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-NC-20181016_109-0" class="reference"><a href="#cite_note-NC-20181016-109"><span class="cite-bracket">[</span>105<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-NASA-20181016_110-0" class="reference"><a href="#cite_note-NASA-20181016-110"><span class="cite-bracket">[</span>106<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-SPC-20181017_111-0" class="reference"><a href="#cite_note-SPC-20181017-111"><span class="cite-bracket">[</span>107<span class="cite-bracket">]</span></a></sup> </p><p>In July 2019, astronomers reported that a new method to determine the <a href="/wiki/Hubble_constant" class="mw-redirect" title="Hubble constant">Hubble constant</a>, and resolve the discrepancy of earlier methods, has been proposed based on the mergers of pairs of neutron stars, following the detection of the neutron star merger of GW170817.<sup id="cite_ref-EA-20190708_112-0" class="reference"><a href="#cite_note-EA-20190708-112"><span class="cite-bracket">[</span>108<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-NRAO-20190708_113-0" class="reference"><a href="#cite_note-NRAO-20190708-113"><span class="cite-bracket">[</span>109<span class="cite-bracket">]</span></a></sup> Their measurement of the Hubble constant is <span class="nowrap"><span data-sort-value="7001703000000000000♠"></span>70.3<span style="margin-left:0.3em;"><span style="display:inline-block;margin-bottom:-0.3em;vertical-align:-0.4em;line-height:1.2em;font-size:85%;text-align:right;">+5.3<br />−5.0</span></span></span> (km/s)/Mpc.<sup id="cite_ref-NAT-20190708_114-0" class="reference"><a href="#cite_note-NAT-20190708-114"><span class="cite-bracket">[</span>110<span class="cite-bracket">]</span></a></sup> </p><p>A 2020 study by <a href="/wiki/University_of_Southampton" title="University of Southampton">University of Southampton</a> PhD student Fabian Gittins suggested that surface irregularities ("mountains") may only be fractions of a millimeter tall (about 0.000003% of the neutron star's diameter), hundreds of times smaller than previously predicted, a result bearing implications for the non-detection of gravitational waves from spinning neutron stars.<sup id="cite_ref-mt-ls_58-1" class="reference"><a href="#cite_note-mt-ls-58"><span class="cite-bracket">[</span>55<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-mt-syfy_115-0" class="reference"><a href="#cite_note-mt-syfy-115"><span class="cite-bracket">[</span>111<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-gittins_116-0" class="reference"><a href="#cite_note-gittins-116"><span class="cite-bracket">[</span>112<span class="cite-bracket">]</span></a></sup> </p><p>Using the <a href="/wiki/James_Webb_Space_Telescope" title="James Webb Space Telescope">JWST</a>, astronomers have identified a neutron star within the remnants of the <a href="/wiki/Supernova_1987A" class="mw-redirect" title="Supernova 1987A">Supernova 1987A</a> <a href="/wiki/Stellar_explosion" class="mw-redirect" title="Stellar explosion">stellar explosion</a> after seeking to do so for 37 years, according to a 23 February 2024 <i><a href="/wiki/Science_(journal)" title="Science (journal)">Science</a></i> article. In a paradigm shift, new JWST data provides the elusive direct confirmation of neutron stars within supernova remnants as well as a deeper understanding of the processes at play within SN 1987A's remnants.<sup id="cite_ref-Fransson_20240223_117-0" class="reference"><a href="#cite_note-Fransson_20240223-117"><span class="cite-bracket">[</span>113<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading2"><h2 id="Subtypes">Subtypes</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=28" title="Edit section: Subtypes"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:PIA23863-NeutronStarTypes-20200624.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/a/a4/PIA23863-NeutronStarTypes-20200624.jpg/220px-PIA23863-NeutronStarTypes-20200624.jpg" decoding="async" width="220" height="343" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/a/a4/PIA23863-NeutronStarTypes-20200624.jpg/330px-PIA23863-NeutronStarTypes-20200624.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/a/a4/PIA23863-NeutronStarTypes-20200624.jpg/440px-PIA23863-NeutronStarTypes-20200624.jpg 2x" data-file-width="1651" data-file-height="2575" /></a><figcaption>Different Types of Neutron Stars</figcaption></figure> <figure class="mw-default-size mw-halign-right" typeof="mw:File/Thumb"><a href="/wiki/File:Neutron_star_magnetic_fields_simulation.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/d/d7/Neutron_star_magnetic_fields_simulation.jpg/220px-Neutron_star_magnetic_fields_simulation.jpg" decoding="async" width="220" height="175" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/d/d7/Neutron_star_magnetic_fields_simulation.jpg/330px-Neutron_star_magnetic_fields_simulation.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/d/d7/Neutron_star_magnetic_fields_simulation.jpg/440px-Neutron_star_magnetic_fields_simulation.jpg 2x" data-file-width="6875" data-file-height="5479" /></a><figcaption>Computer renders of a neutron star with <a href="/wiki/Accretion_disk" title="Accretion disk">accretion disk</a>, with magnetic field lines projected, showing <a href="/wiki/X-ray_burster" title="X-ray burster">bursts of powerful X-rays</a>. The simulations are taken from 2017 data from NASA's NuSTAR and Swift, and ESA's XMM-Newton observatories.</figcaption></figure> <p>There are a number of types of object that consist of or contain a neutron star: </p> <ul><li>Isolated neutron star (INS):<sup id="cite_ref-pavlov_63-3" class="reference"><a href="#cite_note-pavlov-63"><span class="cite-bracket">[</span>60<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-cco_66-2" class="reference"><a href="#cite_note-cco-66"><span class="cite-bracket">[</span>63<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-ins_118-0" class="reference"><a href="#cite_note-ins-118"><span class="cite-bracket">[</span>114<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-slac_119-0" class="reference"><a href="#cite_note-slac-119"><span class="cite-bracket">[</span>115<span class="cite-bracket">]</span></a></sup> not in a binary system. <ul><li><a href="/wiki/Rotation-powered_pulsar" class="mw-redirect" title="Rotation-powered pulsar">Rotation-powered pulsar</a> (RPP or "radio pulsar"):<sup id="cite_ref-cco_66-3" class="reference"><a href="#cite_note-cco-66"><span class="cite-bracket">[</span>63<span class="cite-bracket">]</span></a></sup> neutron stars that emit directed pulses of radiation towards us at regular intervals (due to their strong magnetic fields). <ul><li><a href="/wiki/Rotating_radio_transient" title="Rotating radio transient">Rotating radio transient</a> (RRATs):<sup id="cite_ref-cco_66-4" class="reference"><a href="#cite_note-cco-66"><span class="cite-bracket">[</span>63<span class="cite-bracket">]</span></a></sup> are thought to be pulsars which emit more sporadically and/or with higher pulse-to-pulse variability than the bulk of the known pulsars.</li></ul></li> <li><a href="/wiki/Magnetar" title="Magnetar">Magnetar</a>: a neutron star with an extremely strong magnetic field (1000 times more than a regular neutron star), and long rotation periods (5 to 12 seconds). <ul><li><a href="/wiki/Soft_gamma_repeater" title="Soft gamma repeater">Soft gamma repeater</a> (SGR).<sup id="cite_ref-pavlov_63-4" class="reference"><a href="#cite_note-pavlov-63"><span class="cite-bracket">[</span>60<span class="cite-bracket">]</span></a></sup></li> <li><a href="/wiki/Anomalous_X-ray_pulsar" title="Anomalous X-ray pulsar">Anomalous X-ray pulsar</a> (AXP).<sup id="cite_ref-pavlov_63-5" class="reference"><a href="#cite_note-pavlov-63"><span class="cite-bracket">[</span>60<span class="cite-bracket">]</span></a></sup></li></ul></li> <li><a href="/wiki/Radio-quiet_neutron_star" title="Radio-quiet neutron star">Radio-quiet neutron stars</a>. <ul><li>X-ray dim isolated neutron stars.<sup id="cite_ref-cco_66-5" class="reference"><a href="#cite_note-cco-66"><span class="cite-bracket">[</span>63<span class="cite-bracket">]</span></a></sup></li> <li><a href="/wiki/Central_compact_object" title="Central compact object">Central compact objects</a> in <a href="/wiki/Supernova_remnant" title="Supernova remnant">supernova remnants</a> (CCOs in SNRs): young, radio-quiet non-pulsating X-ray sources, thought to be Isolated Neutron Stars surrounded by supernova remnants.<sup id="cite_ref-cco_66-6" class="reference"><a href="#cite_note-cco-66"><span class="cite-bracket">[</span>63<span class="cite-bracket">]</span></a></sup></li></ul></li></ul></li> <li><a href="/wiki/X-ray_pulsar" title="X-ray pulsar">X-ray pulsars</a> or "accretion-powered pulsars": a class of <a href="/wiki/X-ray_binaries" class="mw-redirect" title="X-ray binaries">X-ray binaries</a>. <ul><li>Low-mass X-ray binary pulsars: a class of <a href="/wiki/Low-mass_X-ray_binaries" class="mw-redirect" title="Low-mass X-ray binaries">low-mass X-ray binaries</a> (LMXB), a pulsar with a main sequence star, white dwarf or red giant. <ul><li><a href="/wiki/Millisecond_pulsar" title="Millisecond pulsar">Millisecond pulsar</a> (MSP) ("recycled pulsar"). <ul><li>"Spider Pulsar", a pulsar where their companion is a semi-degenerate star.<sup id="cite_ref-120" class="reference"><a href="#cite_note-120"><span class="cite-bracket">[</span>116<span class="cite-bracket">]</span></a></sup> <ul><li>"Black Widow" pulsar, a pulsar that falls under the "Spider Pulsar" if the companion has extremely low mass (less than 0.1 <var>M</var><sub>☉</sub>).</li> <li>"Redback" pulsar, are if the companion is more massive.</li></ul></li> <li>Sub-millisecond pulsar.<sup id="cite_ref-121" class="reference"><a href="#cite_note-121"><span class="cite-bracket">[</span>117<span class="cite-bracket">]</span></a></sup></li></ul></li> <li><a href="/wiki/X-ray_burster" title="X-ray burster">X-ray burster</a>: a neutron star with a low mass binary companion from which matter is accreted resulting in irregular bursts of energy from the surface of the neutron star.</li></ul></li> <li>Intermediate-mass X-ray binary pulsars: a class of <a href="/wiki/Intermediate-mass_X-ray_binaries" class="mw-redirect" title="Intermediate-mass X-ray binaries">intermediate-mass X-ray binaries</a> (IMXB), a pulsar with an intermediate mass star.</li> <li>High-mass X-ray binary pulsars: a class of <a href="/wiki/High-mass_X-ray_binaries" class="mw-redirect" title="High-mass X-ray binaries">high-mass X-ray binaries</a> (HMXB), a pulsar with a massive star.</li> <li><a href="/wiki/Binary_pulsar" title="Binary pulsar">Binary pulsars</a>: a <a href="/wiki/Pulsar" title="Pulsar">pulsar</a> with a <a href="/wiki/Binary_star" title="Binary star">binary companion</a>, often a <a href="/wiki/White_dwarf" title="White dwarf">white dwarf</a> or neutron star.</li> <li>X-ray tertiary (theorized).<sup id="cite_ref-122" class="reference"><a href="#cite_note-122"><span class="cite-bracket">[</span>118<span class="cite-bracket">]</span></a></sup></li></ul></li></ul> <p>There are also a number of theorized compact stars with similar properties that are not actually neutron stars. </p> <ul><li>Protoneutron star (PNS),<sup id="cite_ref-123" class="reference"><a href="#cite_note-123"><span class="cite-bracket">[</span>119<span class="cite-bracket">]</span></a></sup> a theorized intermediate–stage object that cools and contracts to form a neutron star or a black hole<sup id="cite_ref-124" class="reference"><a href="#cite_note-124"><span class="cite-bracket">[</span>120<span class="cite-bracket">]</span></a></sup></li> <li><a href="/wiki/Exotic_star" title="Exotic star">Exotic star</a> <ul><li><a href="/wiki/Thorne%E2%80%93%C5%BBytkow_object" title="Thorne–Żytkow object">Thorne–Żytkow object</a>: currently a hypothetical merger of a neutron star into a red giant star.</li> <li><a href="/wiki/Quark_star" title="Quark star">Quark star</a>: currently a hypothetical type of neutron star composed of <a href="/wiki/Quark_matter" class="mw-redirect" title="Quark matter">quark matter</a>, or <a href="/wiki/Strange_matter" title="Strange matter">strange matter</a>. As of 2018, there are three candidates.</li> <li><a href="/wiki/Electroweak_star" class="mw-redirect" title="Electroweak star">Electroweak star</a>: currently a hypothetical type of extremely heavy neutron star, in which the quarks are converted to leptons through the electroweak force, but the gravitational collapse of the neutron star is prevented by radiation pressure. As of 2018, there is no evidence for their existence.</li> <li><a href="/wiki/Preon_star" class="mw-redirect" title="Preon star">Preon star</a>: currently a hypothetical type of neutron star composed of <a href="/wiki/Preon_matter" class="mw-redirect" title="Preon matter">preon matter</a>. As of 2018, there is no evidence for the existence of <a href="/wiki/Preon" title="Preon">preons</a>.</li></ul></li></ul> <div class="mw-heading mw-heading2"><h2 id="Examples_of_neutron_stars">Examples of neutron stars</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=29" title="Edit section: Examples of neutron stars"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Artist%27s_concept_of_PSR_B1257%2B12_system.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/7/7c/Artist%27s_concept_of_PSR_B1257%2B12_system.jpg/220px-Artist%27s_concept_of_PSR_B1257%2B12_system.jpg" decoding="async" width="220" height="176" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/7/7c/Artist%27s_concept_of_PSR_B1257%2B12_system.jpg/330px-Artist%27s_concept_of_PSR_B1257%2B12_system.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/7/7c/Artist%27s_concept_of_PSR_B1257%2B12_system.jpg/440px-Artist%27s_concept_of_PSR_B1257%2B12_system.jpg 2x" data-file-width="3000" data-file-height="2400" /></a><figcaption>An artist's conception of the pulsar planet <a href="/wiki/PSR_B1257%2B12_C" title="PSR B1257+12 C">PSR B1257+12 C</a>, with bright aurorae</figcaption></figure> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236090951"><div role="note" class="hatnote navigation-not-searchable">See also: <a href="/wiki/Pulsar#Significant_pulsars" title="Pulsar">Pulsar § Significant pulsars</a></div> <ul><li><a href="/wiki/Black_Widow_Pulsar" title="Black Widow Pulsar">Black Widow Pulsar</a> – a millisecond pulsar that is very massive</li> <li><a href="/wiki/PSR_J0952-0607" class="mw-redirect" title="PSR J0952-0607">PSR J0952-0607</a> – the heaviest neutron star with <span class="nowrap"><span data-sort-value="7000235000000000000♠"></span>2.35<span style="margin-left:0.3em;"><span style="display:inline-block;margin-bottom:-0.3em;vertical-align:-0.4em;line-height:1.2em;font-size:85%;text-align:right;">+0.17<br />−0.17</span></span></span> <var>M</var><sub>☉</sub>, a type of Black Widow Pulsar<sup id="cite_ref-blackwidow_8-1" class="reference"><a href="#cite_note-blackwidow-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-125" class="reference"><a href="#cite_note-125"><span class="cite-bracket">[</span>121<span class="cite-bracket">]</span></a></sup></li> <li><a href="/wiki/LGM-1" class="mw-redirect" title="LGM-1">LGM-1</a> (now known as PSR B1919+21) – the first recognized radio-pulsar. It was discovered by <a href="/wiki/Jocelyn_Bell_Burnell" title="Jocelyn Bell Burnell">Jocelyn Bell Burnell</a> in 1967.</li> <li><a href="/wiki/PSR_B1257%2B12" title="PSR B1257+12">PSR B1257+12</a> (Also known as Lich) – the first neutron star discovered with planets (a millisecond pulsar).</li> <li><a href="/wiki/PSR_B1509%E2%88%9258" title="PSR B1509−58">PSR B1509−58</a> – source of the "Hand of God" photo shot by the <a href="/wiki/Chandra_X-ray_Observatory" title="Chandra X-ray Observatory">Chandra X-ray Observatory</a></li> <li><a href="/wiki/RX_J1856.5%E2%88%923754" title="RX J1856.5−3754">RX J1856.5−3754</a> – the closest neutron star</li> <li><a href="/wiki/The_Magnificent_Seven_(neutron_stars)" title="The Magnificent Seven (neutron stars)">The Magnificent Seven</a> – a group of nearby, X-ray dim isolated neutron stars</li> <li><a href="/wiki/PSR_J0348%2B0432" title="PSR J0348+0432">PSR J0348+0432</a> – the most massive neutron star with a well-constrained mass, <span class="nowrap"><span data-sort-value="7000200999999999999♠"></span>2.01<span style="margin-left:0.3em;margin-right:0.15em;">±</span>0.04</span> <var>M</var><sub>☉</sub></li> <li><a href="/wiki/SWIFT_J1756.9-2508" class="mw-redirect" title="SWIFT J1756.9-2508">SWIFT J1756.9-2508</a> – a millisecond pulsar with a stellar-type companion with planetary range mass (below brown dwarf)</li> <li><a href="/wiki/Swift_J1818.0-1607" class="mw-redirect" title="Swift J1818.0-1607">Swift J1818.0-1607</a> – the youngest-known magnetar</li></ul> <div class="mw-heading mw-heading2"><h2 id="Gallery">Gallery</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=30" title="Edit section: Gallery"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <ul class="gallery mw-gallery-packed center"> <li class="gallerybox" style="width: 215.33333333333px"> <div class="thumb" style="width: 213.33333333333px;"><span typeof="mw:File"><span><video id="mwe_player_0" poster="//upload.wikimedia.org/wikipedia/commons/thumb/6/60/Neutron_Star_Manhattan.ogv/320px--Neutron_Star_Manhattan.ogv.jpg" controls="" preload="none" data-mw-tmh="" class="mw-file-element" width="214" height="120" data-durationhint="11" data-mwtitle="Neutron_Star_Manhattan.ogv" data-mwprovider="wikimediacommons"><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/6/60/Neutron_Star_Manhattan.ogv/Neutron_Star_Manhattan.ogv.480p.vp9.webm" type="video/webm; codecs="vp9, opus"" data-transcodekey="480p.vp9.webm" data-width="854" data-height="480" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/6/60/Neutron_Star_Manhattan.ogv/Neutron_Star_Manhattan.ogv.720p.vp9.webm" type="video/webm; codecs="vp9, opus"" data-transcodekey="720p.vp9.webm" data-width="1280" data-height="720" /><source src="//upload.wikimedia.org/wikipedia/commons/6/60/Neutron_Star_Manhattan.ogv" type="video/ogg; codecs="theora"" data-width="1280" data-height="720" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/6/60/Neutron_Star_Manhattan.ogv/Neutron_Star_Manhattan.ogv.144p.mjpeg.mov" type="video/quicktime" data-transcodekey="144p.mjpeg.mov" data-width="256" data-height="144" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/6/60/Neutron_Star_Manhattan.ogv/Neutron_Star_Manhattan.ogv.240p.vp9.webm" type="video/webm; codecs="vp9, opus"" data-transcodekey="240p.vp9.webm" data-width="426" data-height="240" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/6/60/Neutron_Star_Manhattan.ogv/Neutron_Star_Manhattan.ogv.360p.webm" type="video/webm; codecs="vp8, vorbis"" data-transcodekey="360p.webm" data-width="640" data-height="360" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/6/60/Neutron_Star_Manhattan.ogv/Neutron_Star_Manhattan.ogv.360p.vp9.webm" type="video/webm; codecs="vp9, opus"" data-transcodekey="360p.vp9.webm" data-width="640" data-height="360" /></video></span></span></div> <div class="gallerytext">Neutron stars containing 500,000 Earth-masses in 25-kilometer-diameter (16 mi) sphere</div> </li> <li class="gallerybox" style="width: 215.33333333333px"> <div class="thumb" style="width: 213.33333333333px;"><span typeof="mw:File"><span><video id="mwe_player_1" poster="//upload.wikimedia.org/wikipedia/commons/thumb/0/06/Crash_and_Burst.ogv/320px--Crash_and_Burst.ogv.jpg" controls="" preload="none" data-mw-tmh="" class="mw-file-element" width="214" height="120" data-durationhint="208" data-mwtitle="Crash_and_Burst.ogv" data-mwprovider="wikimediacommons"><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/0/06/Crash_and_Burst.ogv/Crash_and_Burst.ogv.480p.vp9.webm" type="video/webm; codecs="vp9, opus"" data-transcodekey="480p.vp9.webm" data-width="854" data-height="480" /><source src="//upload.wikimedia.org/wikipedia/commons/0/06/Crash_and_Burst.ogv" type="video/ogg; codecs="theora, vorbis"" data-width="960" data-height="540" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/0/06/Crash_and_Burst.ogv/Crash_and_Burst.ogv.144p.mjpeg.mov" type="video/quicktime" data-transcodekey="144p.mjpeg.mov" data-width="256" data-height="144" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/0/06/Crash_and_Burst.ogv/Crash_and_Burst.ogv.240p.vp9.webm" type="video/webm; codecs="vp9, opus"" data-transcodekey="240p.vp9.webm" data-width="426" data-height="240" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/0/06/Crash_and_Burst.ogv/Crash_and_Burst.ogv.360p.webm" type="video/webm; codecs="vp8, vorbis"" data-transcodekey="360p.webm" data-width="640" data-height="360" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/0/06/Crash_and_Burst.ogv/Crash_and_Burst.ogv.360p.vp9.webm" type="video/webm; codecs="vp9, opus"" data-transcodekey="360p.vp9.webm" data-width="640" data-height="360" /><track src="https://commons.wikimedia.org/w/api.php?action=timedtext&title=File%3ACrash_and_Burst.ogv&lang=en&trackformat=vtt&origin=%2A" kind="subtitles" type="text/vtt" srclang="en" label="English ‪(en)‬" data-dir="ltr" /><track src="https://commons.wikimedia.org/w/api.php?action=timedtext&title=File%3ACrash_and_Burst.ogv&lang=ko&trackformat=vtt&origin=%2A" kind="subtitles" type="text/vtt" srclang="ko" label="한국어 ‪(ko)‬" data-dir="ltr" /><track src="https://commons.wikimedia.org/w/api.php?action=timedtext&title=File%3ACrash_and_Burst.ogv&lang=mk&trackformat=vtt&origin=%2A" kind="subtitles" type="text/vtt" srclang="mk" label="македонски ‪(mk)‬" data-dir="ltr" /></video></span></span></div> <div class="gallerytext"><a href="/wiki/Neutron_star_collision" class="mw-redirect" title="Neutron star collision">Neutron stars colliding</a></div> </li> <li class="gallerybox" style="width: 178px"> <div class="thumb" style="width: 176px;"><span typeof="mw:File"><span><video id="mwe_player_2" poster="//upload.wikimedia.org/wikipedia/commons/thumb/4/44/Neutron_star_collision.ogv/264px--Neutron_star_collision.ogv.jpg" controls="" preload="none" data-mw-tmh="" class="mw-file-element" width="176" height="120" data-durationhint="24" data-mwtitle="Neutron_star_collision.ogv" data-mwprovider="wikimediacommons"><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/4/44/Neutron_star_collision.ogv/Neutron_star_collision.ogv.240p.vp9.webm" type="video/webm; codecs="vp9, opus"" data-transcodekey="240p.vp9.webm" data-width="352" data-height="240" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/4/44/Neutron_star_collision.ogv/Neutron_star_collision.ogv.360p.webm" type="video/webm; codecs="vp8, vorbis"" data-transcodekey="360p.webm" data-width="352" data-height="240" /><source src="//upload.wikimedia.org/wikipedia/commons/4/44/Neutron_star_collision.ogv" type="video/ogg; codecs="theora"" data-width="352" data-height="240" /><source src="//upload.wikimedia.org/wikipedia/commons/transcoded/4/44/Neutron_star_collision.ogv/Neutron_star_collision.ogv.144p.mjpeg.mov" type="video/quicktime" data-transcodekey="144p.mjpeg.mov" data-width="212" data-height="144" /></video></span></span></div> <div class="gallerytext">Neutron star collision</div> </li> <li class="gallerybox" style="width: 104px"> <div class="thumb" style="width: 102px;"><span typeof="mw:File"><a href="/wiki/File:Neutron_Star_simulation.png" class="mw-file-description" title="Artist's impression of a neutron star bending light"><img alt="Artist's impression of a neutron star bending light" src="//upload.wikimedia.org/wikipedia/commons/thumb/1/1d/Neutron_Star_simulation.png/153px-Neutron_Star_simulation.png" decoding="async" width="102" height="120" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/1/1d/Neutron_Star_simulation.png/230px-Neutron_Star_simulation.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/1/1d/Neutron_Star_simulation.png/307px-Neutron_Star_simulation.png 2x" data-file-width="1536" data-file-height="1802" /></a></span></div> <div class="gallerytext">Artist's impression of a neutron star bending light</div> </li> </ul> <div class="mw-heading mw-heading2"><h2 id="See_also">See also</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=31" title="Edit section: See also"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <style data-mw-deduplicate="TemplateStyles:r1184024115">.mw-parser-output .div-col{margin-top:0.3em;column-width:30em}.mw-parser-output .div-col-small{font-size:90%}.mw-parser-output .div-col-rules{column-rule:1px solid #aaa}.mw-parser-output .div-col dl,.mw-parser-output .div-col ol,.mw-parser-output .div-col ul{margin-top:0}.mw-parser-output .div-col li,.mw-parser-output .div-col dd{page-break-inside:avoid;break-inside:avoid-column}</style><div class="div-col div-col-small" style="column-width: 20em;"> <ul><li><a href="/wiki/IRAS_00500%2B6713" title="IRAS 00500+6713">IRAS 00500+6713</a> (in 10,000 y)</li> <li><a href="/wiki/Neutron_star_merger" title="Neutron star merger">Neutron star merger</a></li> <li><a href="/wiki/Neutron_stars_in_fiction" title="Neutron stars in fiction">Neutron stars in fiction</a> <ul><li><a href="/wiki/Stars_in_fiction#Neutron_stars" title="Stars in fiction">Stars in fiction § Neutron stars</a></li></ul></li> <li><a href="/wiki/Neutronium" title="Neutronium">Neutronium</a></li> <li><a href="/wiki/Planck_star" title="Planck star">Planck star</a></li> <li><a href="/wiki/Degenerate_matter#Preon_degeneracy_hypothesis" title="Degenerate matter">Preon-degenerate matter</a></li> <li><a href="/wiki/Rotating_radio_transient" title="Rotating radio transient">Rotating radio transient</a></li></ul> </div> <div class="mw-heading mw-heading2"><h2 id="Notes">Notes</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=32" title="Edit section: Notes"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <style data-mw-deduplicate="TemplateStyles:r1239543626">.mw-parser-output .reflist{margin-bottom:0.5em;list-style-type:decimal}@media screen{.mw-parser-output .reflist{font-size:90%}}.mw-parser-output .reflist .references{font-size:100%;margin-bottom:0;list-style-type:inherit}.mw-parser-output .reflist-columns-2{column-width:30em}.mw-parser-output .reflist-columns-3{column-width:25em}.mw-parser-output .reflist-columns{margin-top:0.3em}.mw-parser-output .reflist-columns ol{margin-top:0}.mw-parser-output .reflist-columns li{page-break-inside:avoid;break-inside:avoid-column}.mw-parser-output .reflist-upper-alpha{list-style-type:upper-alpha}.mw-parser-output .reflist-upper-roman{list-style-type:upper-roman}.mw-parser-output .reflist-lower-alpha{list-style-type:lower-alpha}.mw-parser-output .reflist-lower-greek{list-style-type:lower-greek}.mw-parser-output .reflist-lower-roman{list-style-type:lower-roman}</style><div class="reflist reflist-lower-alpha"> <div class="mw-references-wrap"><ol class="references"> <li id="cite_note-24"><span class="mw-cite-backlink"><b><a href="#cite_ref-24">^</a></b></span> <span class="reference-text"><span class="nowrap"><span data-sort-value="7017370000000000000♠"></span>3.7<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>17</sup> kg/m<sup>3</sup></span> derives from mass <span class="nowrap"><span data-sort-value="7030268000000000000♠"></span>2.68<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>30</sup> kg</span> / volume of star of radius 12 km; <span class="nowrap"><span data-sort-value="7017590000000000000♠"></span>5.9<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>17</sup> kg/m<sup>3</sup></span> derives from mass <span class="nowrap"><span data-sort-value="7030420000000000000♠"></span>4.2<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>30</sup> kg</span> per volume of star radius 11.9 km</span> </li> <li id="cite_note-28"><span class="mw-cite-backlink"><b><a href="#cite_ref-28">^</a></b></span> <span class="reference-text">The average density of material in a neutron star of radius 10 km is <span class="nowrap"><span data-sort-value="7018110000000000000♠"></span>1.1<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>12</sup> kg/cm<sup>3</sup></span>. Therefore, 5 ml of such material is <span class="nowrap"><span data-sort-value="7012550000000000000♠"></span>5.5<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>12</sup> kg</span>, or 5,500,000,000 <a href="/wiki/Metric_ton" class="mw-redirect" title="Metric ton">metric tons</a>. This is about 15 times the total mass of the human world population. Alternatively, 5 ml from a neutron star of radius 20 km radius (average density <span class="nowrap"><span data-sort-value="7016835000000000000♠"></span>8.35<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>10</sup> kg/cm<sup>3</sup></span>) has a mass of about 400 million metric tons, or about the mass of all humans. The gravitational field is ca. <span class="nowrap"><span data-sort-value="7011200000000000000♠"></span>2<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>11</sup></span><i>g</i> or ca. <span class="nowrap"><span data-sort-value="7012200000000000000♠"></span>2<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>12</sup></span> N/kg. Moon weight is calculated at 1<i>g</i>.</span> </li> <li id="cite_note-47"><span class="mw-cite-backlink"><b><a href="#cite_ref-47">^</a></b></span> <span class="reference-text">Magnetic <a href="/wiki/Energy_density" title="Energy density">energy density</a> for a <a href="/wiki/Magnetic_field" title="Magnetic field">field B</a> is <span class="nowrap"> U = <style data-mw-deduplicate="TemplateStyles:r1154941027">.mw-parser-output .frac{white-space:nowrap}.mw-parser-output .frac .num,.mw-parser-output .frac .den{font-size:80%;line-height:0;vertical-align:super}.mw-parser-output .frac .den{vertical-align:sub}.mw-parser-output .sr-only{border:0;clip:rect(0,0,0,0);clip-path:polygon(0px 0px,0px 0px,0px 0px);height:1px;margin:-1px;overflow:hidden;padding:0;position:absolute;width:1px}</style><span class="frac"><span class="num"><a href="/wiki/Vacuum_permeability" title="Vacuum permeability">μ<sub>0</sub></a> B<sup>2</sup></span>⁄<span class="den">2</span></span> .</span><sup id="cite_ref-46" class="reference"><a href="#cite_note-46"><span class="cite-bracket">[</span>44<span class="cite-bracket">]</span></a></sup> Substituting <span class="nowrap"> B = <span class="nowrap"><span data-sort-value="7008100000000000000♠"></span>10<sup>8</sup> T</span> ,</span> get <span class="nowrap">U = <span class="nowrap"><span data-sort-value="7021400000000000000♠"></span>4<span style="margin-left:0.25em;margin-right:0.15em;">×</span>10<sup>21</sup> J/m<sup>3</sup></span> .</span> Dividing by c<sup>2</sup> one obtains the equivalent mass density of <span class="nowrap"><span data-sort-value="7004445000000000000♠"></span>44<span style="margin-left:.25em;">500</span> kg/m<sup>3</sup></span>, which exceeds the <a href="/wiki/Standard_temperature_and_pressure" title="Standard temperature and pressure">standard temperature and pressure</a> density of all known materials. Compare with <span class="nowrap"><span data-sort-value="7004225900000000000♠"></span>22<span style="margin-left:.25em;">590</span> kg/m<sup>3</sup></span> for <a href="/wiki/Osmium" title="Osmium">osmium</a>, the densest stable element.</span> </li> <li id="cite_note-93"><span class="mw-cite-backlink"><b><a href="#cite_ref-93">^</a></b></span> <span class="reference-text">Even before the discovery of neutron, in 1931, neutron stars were <i>anticipated</i> by <a href="/wiki/Lev_Landau" title="Lev Landau">Lev Landau</a>, who wrote about stars where "atomic nuclei come in close contact, forming one gigantic nucleus".<sup id="cite_ref-91" class="reference"><a href="#cite_note-91"><span class="cite-bracket">[</span>88<span class="cite-bracket">]</span></a></sup> However, the widespread opinion that Landau <i>predicted</i> neutron stars proves to be wrong.<sup id="cite_ref-92" class="reference"><a href="#cite_note-92"><span class="cite-bracket">[</span>89<span class="cite-bracket">]</span></a></sup></span> </li> </ol></div></div> <div class="mw-heading mw-heading2"><h2 id="References">References</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=33" title="Edit section: References"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1239543626"><div class="reflist"> <div class="mw-references-wrap mw-references-columns"><ol class="references"> <li id="cite_note-1"><span class="mw-cite-backlink"><b><a href="#cite_ref-1">^</a></b></span> <span class="reference-text"><style data-mw-deduplicate="TemplateStyles:r1238218222">.mw-parser-output cite.citation{font-style:inherit;word-wrap:break-word}.mw-parser-output .citation q{quotes:"\"""\"""'""'"}.mw-parser-output .citation:target{background-color:rgba(0,127,255,0.133)}.mw-parser-output .id-lock-free.id-lock-free a{background:url("//upload.wikimedia.org/wikipedia/commons/6/65/Lock-green.svg")right 0.1em center/9px no-repeat}.mw-parser-output .id-lock-limited.id-lock-limited a,.mw-parser-output .id-lock-registration.id-lock-registration a{background:url("//upload.wikimedia.org/wikipedia/commons/d/d6/Lock-gray-alt-2.svg")right 0.1em center/9px no-repeat}.mw-parser-output .id-lock-subscription.id-lock-subscription a{background:url("//upload.wikimedia.org/wikipedia/commons/a/aa/Lock-red-alt-2.svg")right 0.1em center/9px no-repeat}.mw-parser-output .cs1-ws-icon a{background:url("//upload.wikimedia.org/wikipedia/commons/4/4c/Wikisource-logo.svg")right 0.1em center/12px no-repeat}body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .id-lock-free a,body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .id-lock-limited a,body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .id-lock-registration a,body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .id-lock-subscription a,body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .cs1-ws-icon a{background-size:contain;padding:0 1em 0 0}.mw-parser-output .cs1-code{color:inherit;background:inherit;border:none;padding:inherit}.mw-parser-output .cs1-hidden-error{display:none;color:var(--color-error,#d33)}.mw-parser-output .cs1-visible-error{color:var(--color-error,#d33)}.mw-parser-output .cs1-maint{display:none;color:#085;margin-left:0.3em}.mw-parser-output .cs1-kern-left{padding-left:0.2em}.mw-parser-output .cs1-kern-right{padding-right:0.2em}.mw-parser-output .citation .mw-selflink{font-weight:inherit}@media screen{.mw-parser-output .cs1-format{font-size:95%}html.skin-theme-clientpref-night .mw-parser-output .cs1-maint{color:#18911f}}@media screen and (prefers-color-scheme:dark){html.skin-theme-clientpref-os .mw-parser-output .cs1-maint{color:#18911f}}</style><cite id="CITEREFGlendenning2012" class="citation book cs1">Glendenning, Norman K. (2012). <a rel="nofollow" class="external text" href="https://books.google.com/books?id=cCDlBwAAQBAJ&pg=PA1"><i>Compact Stars: Nuclear Physics, Particle Physics and General Relativity</i></a> (illustrated ed.). Springer Science & Business Media. p. 1. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-1-4684-0491-3" title="Special:BookSources/978-1-4684-0491-3"><bdi>978-1-4684-0491-3</bdi></a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20170131202613/https://books.google.com/books?id=cCDlBwAAQBAJ&pg=PA1">Archived</a> from the original on 2017-01-31<span class="reference-accessdate">. Retrieved <span class="nowrap">2016-03-21</span></span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Compact+Stars%3A+Nuclear+Physics%2C+Particle+Physics+and+General+Relativity&rft.pages=1&rft.edition=illustrated&rft.pub=Springer+Science+%26+Business+Media&rft.date=2012&rft.isbn=978-1-4684-0491-3&rft.aulast=Glendenning&rft.aufirst=Norman+K.&rft_id=https%3A%2F%2Fbooks.google.com%2Fbooks%3Fid%3DcCDlBwAAQBAJ%26pg%3DPA1&rfr_id=info%3Asid%2Fen.wikipedia.org%3ANeutron+star" class="Z3988"></span></span> </li> <li id="cite_note-2"><span class="mw-cite-backlink"><b><a href="#cite_ref-2">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFSeedsBackman2009" class="citation book cs1">Seeds, Michael; Backman, Dana (2009). <a rel="nofollow" class="external text" href="https://books.google.com/books?id=DajpkyXS-NUC&pg=PT356"><i>Astronomy: The Solar System and Beyond</i></a> (6th ed.). Cengage Learning. p. 339. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-0-495-56203-0" title="Special:BookSources/978-0-495-56203-0"><bdi>978-0-495-56203-0</bdi></a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20210206222508/https://books.google.com/books?id=DajpkyXS-NUC&pg=PT356">Archived</a> from the original on 2021-02-06<span class="reference-accessdate">. Retrieved <span class="nowrap">2018-02-22</span></span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Astronomy%3A+The+Solar+System+and+Beyond&rft.pages=339&rft.edition=6th&rft.pub=Cengage+Learning&rft.date=2009&rft.isbn=978-0-495-56203-0&rft.aulast=Seeds&rft.aufirst=Michael&rft.au=Backman%2C+Dana&rft_id=https%3A%2F%2Fbooks.google.com%2Fbooks%3Fid%3DDajpkyXS-NUC%26pg%3DPT356&rfr_id=info%3Asid%2Fen.wikipedia.org%3ANeutron+star" class="Z3988"></span></span> </li> <li id="cite_note-3"><span class="mw-cite-backlink"><b><a href="#cite_ref-3">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFHegerFryerWoosleyLanger2003" class="citation journal cs1">Heger, A.; Fryer, C. L.; Woosley, S. E.; Langer, N.; Hartmann, D. H. (2003). "How Massive Single Stars End Their Life". <i><a href="/wiki/Astrophysical_Journal" class="mw-redirect" title="Astrophysical Journal">Astrophysical Journal</a></i>. <b>591</b> (1): <span class="nowrap">288–</span>300. <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<span class="id-lock-free" title="Freely accessible"><a rel="nofollow" class="external text" href="https://arxiv.org/abs/astro-ph/0212469">astro-ph/0212469</a></span>. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2003ApJ...591..288H">2003ApJ...591..288H</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1086%2F375341">10.1086/375341</a>. <a href="/wiki/S2CID_(identifier)" class="mw-redirect" title="S2CID (identifier)">S2CID</a> <a rel="nofollow" class="external text" href="https://api.semanticscholar.org/CorpusID:59065632">59065632</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Astrophysical+Journal&rft.atitle=How+Massive+Single+Stars+End+Their+Life&rft.volume=591&rft.issue=1&rft.pages=%3Cspan+class%3D%22nowrap%22%3E288-%3C%2Fspan%3E300&rft.date=2003&rft_id=info%3Aarxiv%2Fastro-ph%2F0212469&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A59065632%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.1086%2F375341&rft_id=info%3Abibcode%2F2003ApJ...591..288H&rft.aulast=Heger&rft.aufirst=A.&rft.au=Fryer%2C+C.+L.&rft.au=Woosley%2C+S.+E.&rft.au=Langer%2C+N.&rft.au=Hartmann%2C+D.+H.&rfr_id=info%3Asid%2Fen.wikipedia.org%3ANeutron+star" class="Z3988"></span></span> </li> <li id="cite_note-4"><span class="mw-cite-backlink"><b><a href="#cite_ref-4">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFTolman1939" class="citation journal cs1">Tolman, R. 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(1939). <a rel="nofollow" class="external text" href="https://authors.library.caltech.edu/4362/1/TOLpr39.pdf">"Static Solutions of Einstein's Field Equations for Spheres of Fluid"</a> <span class="cs1-format">(PDF)</span>. <i><a href="/wiki/Physical_Review" title="Physical Review">Physical Review</a></i>. <b>55</b> (4): <span class="nowrap">364–</span>373. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1939PhRv...55..364T">1939PhRv...55..364T</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1103%2FPhysRev.55.364">10.1103/PhysRev.55.364</a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20180722071018/https://authors.library.caltech.edu/4362/1/TOLpr39.pdf">Archived</a> <span class="cs1-format">(PDF)</span> from the original on 2018-07-22<span class="reference-accessdate">. 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Retrieved <span class="nowrap">2022-07-25</span></span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=unknown&rft.jtitle=Science+News&rft.atitle=The+heaviest+neutron+star+on+record+is+2.35+times+the+mass+of+the+sun&rft.date=2022-07-22&rft.aulast=Croswell&rft.aufirst=Ken&rft_id=https%3A%2F%2Fwww.sciencenews.org%2Farticle%2Fheaviest-neutron-star-mass-sun-record-black-holes&rfr_id=info%3Asid%2Fen.wikipedia.org%3ANeutron+star" class="Z3988"></span></span> </li> <li id="cite_note-Chandra-9"><span class="mw-cite-backlink"><b><a href="#cite_ref-Chandra_9-0">^</a></b></span> <span class="reference-text">"<a rel="nofollow" class="external text" href="https://Chandra.harvard.edu/resources/faq/sources/snr/snr-39.html">Q&A: Supernova Remnants and Neutron Stars"</a>, <i>Chandra.harvard.edu</i> (September 5, 2008)</span> </li> <li id="cite_note-10"><span class="mw-cite-backlink"><b><a href="#cite_ref-10">^</a></b></span> <span class="reference-text">"Magnetic Hydrogen Atmosphere Models and the Neutron Star RX J1856.5−3754" (<a rel="nofollow" class="external text" href="https://arxiv.org/pdf/astro-ph/0612145v1.pdf">PDF</a>), Wynn C. 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Retrieved <span class="nowrap">2009-10-09</span></span>. <q>Durch die gravitative Lichtablenkung ist mehr als die Hälfte der Oberfläche sichtbar. Masse des Neutronensterns: 1, Radius des Neutronensterns: 4, ... dimensionslosen Einheiten (<i>c</i>, <i>G</i> = 1)</q></cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=Tempolimit+Lichtgeschwindigkeit&rft.date=1990-10-09&rft.aulast=Zahn&rft.aufirst=Corvin&rft_id=http%3A%2F%2Fwww.tempolimit-lichtgeschwindigkeit.de%2Fgalerie%2Fgalerie.html&rfr_id=info%3Asid%2Fen.wikipedia.org%3ANeutron+star" class="Z3988"></span></span> </li> <li id="cite_note-50"><span class="mw-cite-backlink"><b><a href="#cite_ref-50">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFGreenJonesBurnell2004" class="citation book cs1">Green, Simon F.; Jones, Mark H.; Burnell, S. 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Springer Science & Business Media. p. 82. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-0-387-33367-0" title="Special:BookSources/978-0-387-33367-0"><bdi>978-0-387-33367-0</bdi></a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20210206223425/https://books.google.com/books?id=aUjkKuaVIloC&pg=PA82">Archived</a> from the original on 2021-02-06<span class="reference-accessdate">. Retrieved <span class="nowrap">2016-11-29</span></span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=A+Companion+to+Astronomy+and+Astrophysics%3A+Chronology+and+Glossary+with+Data+Tables&rft.pages=82&rft.edition=illustrated&rft.pub=Springer+Science+%26+Business+Media&rft.date=2007&rft.isbn=978-0-387-33367-0&rft.aulast=Lang&rft.aufirst=Kenneth&rft_id=https%3A%2F%2Fbooks.google.com%2Fbooks%3Fid%3DaUjkKuaVIloC%26pg%3DPA82&rfr_id=info%3Asid%2Fen.wikipedia.org%3ANeutron+star" class="Z3988"></span></span> </li> <li id="cite_note-102"><span class="mw-cite-backlink"><b><a href="#cite_ref-102">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFHaenselPotekhinYakovlev2007" class="citation book cs1">Haensel, Paweł; Potekhin, Alexander Y.; Yakovlev, Dmitry G. (2007). <a rel="nofollow" class="external text" href="https://books.google.com/books?id=fgj_TZ06niYC&pg=PA474"><i>Neutron Stars 1: Equation of State and Structure</i></a> (illustrated ed.). Springer Science & Business Media. p. 474. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-0-387-47301-7" title="Special:BookSources/978-0-387-47301-7"><bdi>978-0-387-47301-7</bdi></a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20210206223723/https://books.google.com/books?id=fgj_TZ06niYC&pg=PA474">Archived</a> from the original on 2021-02-06<span class="reference-accessdate">. Retrieved <span class="nowrap">2016-11-29</span></span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Neutron+Stars+1%3A+Equation+of+State+and+Structure&rft.pages=474&rft.edition=illustrated&rft.pub=Springer+Science+%26+Business+Media&rft.date=2007&rft.isbn=978-0-387-47301-7&rft.aulast=Haensel&rft.aufirst=Pawe%C5%82&rft.au=Potekhin%2C+Alexander+Y.&rft.au=Yakovlev%2C+Dmitry+G.&rft_id=https%3A%2F%2Fbooks.google.com%2Fbooks%3Fid%3Dfgj_TZ06niYC%26pg%3DPA474&rfr_id=info%3Asid%2Fen.wikipedia.org%3ANeutron+star" class="Z3988"></span></span> </li> <li id="cite_note-103"><span class="mw-cite-backlink"><b><a href="#cite_ref-103">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFGraham-Smith2006" class="citation book cs1">Graham-Smith, Francis (2006). <a rel="nofollow" class="external text" href="https://books.google.com/books?id=AK9N3zxL4ToC&pg=PA11"><i>Pulsar Astronomy</i></a> (illustrated ed.). Cambridge University Press. p. 11. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-0-521-83954-9" title="Special:BookSources/978-0-521-83954-9"><bdi>978-0-521-83954-9</bdi></a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20210206223536/https://books.google.com/books?id=AK9N3zxL4ToC&pg=PA11">Archived</a> from the original on 2021-02-06<span class="reference-accessdate">. Retrieved <span class="nowrap">2016-11-29</span></span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Pulsar+Astronomy&rft.pages=11&rft.edition=illustrated&rft.pub=Cambridge+University+Press&rft.date=2006&rft.isbn=978-0-521-83954-9&rft.aulast=Graham-Smith&rft.aufirst=Francis&rft_id=https%3A%2F%2Fbooks.google.com%2Fbooks%3Fid%3DAK9N3zxL4ToC%26pg%3DPA11&rfr_id=info%3Asid%2Fen.wikipedia.org%3ANeutron+star" class="Z3988"></span></span> </li> <li id="cite_note-104"><span class="mw-cite-backlink"><b><a href="#cite_ref-104">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFGhosh2007" class="citation book cs1">Ghosh, Pranab (2007). <a rel="nofollow" class="external text" href="https://books.google.com/books?id=fmtqDQAAQBAJ&pg=PA281"><i>Rotation and Accretion Powered Pulsars</i></a> (illustrated ed.). World Scientific. p. 281. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/978-981-02-4744-7" title="Special:BookSources/978-981-02-4744-7"><bdi>978-981-02-4744-7</bdi></a>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20210206223426/https://books.google.com/books?id=fmtqDQAAQBAJ&pg=PA281">Archived</a> from the original on 2021-02-06<span class="reference-accessdate">. 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Retrieved <span class="nowrap">17 November</span> 2017</span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=LIGO+Detection+of+Colliding+Neutron+Stars+Spawns+Global+Effort+to+Study+the+Rare+Event&rft.date=2017-10-16&rft.aulast=Burtnyk&rft.aufirst=Kimberly+M.&rft_id=https%3A%2F%2Fwww.ligo.caltech.edu%2Fnews%2Fligo20171016&rfr_id=info%3Asid%2Fen.wikipedia.org%3ANeutron+star" class="Z3988"></span></span> </li> <li id="cite_note-EA-20181016-108"><span class="mw-cite-backlink"><b><a href="#cite_ref-EA-20181016_108-0">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFUniversity_of_Maryland2018" class="citation news cs1"><a href="/wiki/University_of_Maryland" class="mw-redirect" title="University of Maryland">University of Maryland</a> (16 October 2018). <a rel="nofollow" class="external text" href="https://www.eurekalert.org/pub_releases/2018-10/uom-ait101518.php">"All in the family: Kin of gravitational wave source discovered - New observations suggest that kilonovae -- immense cosmic explosions that produce silver, gold and platinum--may be more common than thought"</a>. <i><a href="/wiki/EurekAlert!" class="mw-redirect" title="EurekAlert!">EurekAlert!</a></i>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20181016142323/https://www.eurekalert.org/pub_releases/2018-10/uom-ait101518.php">Archived</a> from the original on 16 October 2018<span class="reference-accessdate">. Retrieved <span class="nowrap">17 October</span> 2018</span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=EurekAlert%21&rft.atitle=All+in+the+family%3A+Kin+of+gravitational+wave+source+discovered+-+New+observations+suggest+that+kilonovae+--+immense+cosmic+explosions+that+produce+silver%2C+gold+and+platinum--may+be+more+common+than+thought&rft.date=2018-10-16&rft.au=University+of+Maryland&rft_id=https%3A%2F%2Fwww.eurekalert.org%2Fpub_releases%2F2018-10%2Fuom-ait101518.php&rfr_id=info%3Asid%2Fen.wikipedia.org%3ANeutron+star" class="Z3988"></span></span> </li> <li id="cite_note-NC-20181016-109"><span class="mw-cite-backlink"><b><a href="#cite_ref-NC-20181016_109-0">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFTroja,_E.2018" class="citation journal cs1">Troja, E.; et al. 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Retrieved <span class="nowrap">17 October</span> 2018</span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=NASA&rft.atitle=GRB+150101B%3A+A+Distant+Cousin+to+GW170817&rft.date=2018-10-16&rft.aulast=Mohon&rft.aufirst=Lee&rft_id=https%3A%2F%2Fwww.nasa.gov%2Fmission_pages%2Fchandra%2Fimages%2Fgrb-150101b-a-distant-cousin-to-gw170817.html&rfr_id=info%3Asid%2Fen.wikipedia.org%3ANeutron+star" class="Z3988"></span></span> </li> <li id="cite_note-SPC-20181017-111"><span class="mw-cite-backlink"><b><a href="#cite_ref-SPC-20181017_111-0">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFWall2018" class="citation web cs1">Wall, Mike (17 October 2018). <a rel="nofollow" class="external text" href="https://www.space.com/42158-another-neutron-star-crash-detected.html">"Powerful Cosmic Flash Is Likely Another Neutron-Star Merger"</a>. <i><a href="/wiki/Space.com" title="Space.com">Space.com</a></i>. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20181017144255/https://www.space.com/42158-another-neutron-star-crash-detected.html">Archived</a> from the original on 17 October 2018<span class="reference-accessdate">. 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Manchester (Science 2004 304:542)"</a>. <i>scienceweek.com</i>. Astrophysics: On observed pulsars. 2004. Archived from <a rel="nofollow" class="external text" href="http://scienceweek.com/2004/sb040806-1.htm">the original</a> on 14 July 2007<span class="reference-accessdate">. Retrieved <span class="nowrap">6 August</span> 2004</span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=unknown&rft.jtitle=scienceweek.com&rft.atitle=The+following+points+are+made+by+R.N.+Manchester+%28Science+2004+304%3A542%29&rft.date=2004&rft_id=http%3A%2F%2Fscienceweek.com%2F2004%2Fsb040806-1.htm&rfr_id=info%3Asid%2Fen.wikipedia.org%3ANeutron+star" class="Z3988"></span></li> <li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFGlendenningKippenhahnAppenzellerBorner2000" class="citation book cs1">Glendenning, Norman K.; Kippenhahn, R.; Appenzeller, I.; Borner, G.; Harwit, M. (2000). <i>Compact Stars</i> (2nd ed.).</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Compact+Stars&rft.edition=2nd&rft.date=2000&rft.aulast=Glendenning&rft.aufirst=Norman+K.&rft.au=Kippenhahn%2C+R.&rft.au=Appenzeller%2C+I.&rft.au=Borner%2C+G.&rft.au=Harwit%2C+M.&rfr_id=info%3Asid%2Fen.wikipedia.org%3ANeutron+star" class="Z3988"></span></li> <li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFKaaretPrieskornin_'t_ZandBrandt2006" class="citation journal cs1">Kaaret, P.; Prieskorn, Z.; in 't Zand, J.J.M.; Brandt, S.; Lund, N.; Mereghetti, S.; et al. (2006). "Evidence for 1122 Hz X-ray burst oscillations from the neutron-star X-ray transient XTE J1739-285". <i>The Astrophysical Journal</i>. <b>657</b> (2): L97. <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<span class="id-lock-free" title="Freely accessible"><a rel="nofollow" class="external text" href="https://arxiv.org/abs/astro-ph/0611716">astro-ph/0611716</a></span>. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2007ApJ...657L..97K">2007ApJ...657L..97K</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1086%2F513270">10.1086/513270</a>. <a href="/wiki/S2CID_(identifier)" class="mw-redirect" title="S2CID (identifier)">S2CID</a> <a rel="nofollow" class="external text" href="https://api.semanticscholar.org/CorpusID:119405361">119405361</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=The+Astrophysical+Journal&rft.atitle=Evidence+for+1122+Hz+X-ray+burst+oscillations+from+the+neutron-star+X-ray+transient+XTE+J1739-285&rft.volume=657&rft.issue=2&rft.pages=L97&rft.date=2006&rft_id=info%3Aarxiv%2Fastro-ph%2F0611716&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A119405361%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.1086%2F513270&rft_id=info%3Abibcode%2F2007ApJ...657L..97K&rft.aulast=Kaaret&rft.aufirst=P.&rft.au=Prieskorn%2C+Z.&rft.au=in+%27t+Zand%2C+J.J.M.&rft.au=Brandt%2C+S.&rft.au=Lund%2C+N.&rft.au=Mereghetti%2C+S.&rft.au=Gotz%2C+D.&rft.au=Kuulkers%2C+E.&rft.au=Tomsick%2C+J.A.&rfr_id=info%3Asid%2Fen.wikipedia.org%3ANeutron+star" class="Z3988"></span></li></ul> </div> <div class="mw-heading mw-heading2"><h2 id="External_links">External links</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Neutron_star&action=edit&section=35" title="Edit section: External links"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <style data-mw-deduplicate="TemplateStyles:r1235681985">.mw-parser-output .side-box{margin:4px 0;box-sizing:border-box;border:1px solid #aaa;font-size:88%;line-height:1.25em;background-color:var(--background-color-interactive-subtle,#f8f9fa);display:flow-root}.mw-parser-output .side-box-abovebelow,.mw-parser-output .side-box-text{padding:0.25em 0.9em}.mw-parser-output .side-box-image{padding:2px 0 2px 0.9em;text-align:center}.mw-parser-output .side-box-imageright{padding:2px 0.9em 2px 0;text-align:center}@media(min-width:500px){.mw-parser-output .side-box-flex{display:flex;align-items:center}.mw-parser-output .side-box-text{flex:1;min-width:0}}@media(min-width:720px){.mw-parser-output .side-box{width:238px}.mw-parser-output .side-box-right{clear:right;float:right;margin-left:1em}.mw-parser-output .side-box-left{margin-right:1em}}</style><style data-mw-deduplicate="TemplateStyles:r1237033735">@media print{body.ns-0 .mw-parser-output .sistersitebox{display:none!important}}@media screen{html.skin-theme-clientpref-night .mw-parser-output .sistersitebox img[src*="Wiktionary-logo-en-v2.svg"]{background-color:white}}@media screen and (prefers-color-scheme:dark){html.skin-theme-clientpref-os .mw-parser-output .sistersitebox img[src*="Wiktionary-logo-en-v2.svg"]{background-color:white}}</style><div class="side-box side-box-right plainlinks sistersitebox"><style data-mw-deduplicate="TemplateStyles:r1126788409">.mw-parser-output .plainlist ol,.mw-parser-output .plainlist ul{line-height:inherit;list-style:none;margin:0;padding:0}.mw-parser-output .plainlist ol li,.mw-parser-output .plainlist ul li{margin-bottom:0}</style> <div class="side-box-flex"> <div class="side-box-image"><span class="noviewer" typeof="mw:File"><a href="/wiki/File:Commons-logo.svg" class="mw-file-description"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/4/4a/Commons-logo.svg/30px-Commons-logo.svg.png" decoding="async" width="30" height="40" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/4/4a/Commons-logo.svg/45px-Commons-logo.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/4/4a/Commons-logo.svg/59px-Commons-logo.svg.png 2x" data-file-width="1024" data-file-height="1376" /></a></span></div> <div class="side-box-text plainlist">Wikimedia Commons has media related to <span style="font-weight: bold; font-style: italic;"><a href="https://commons.wikimedia.org/wiki/Category:Neutron_stars" class="extiw" title="commons:Category:Neutron stars">Neutron stars</a></span>.</div></div> </div> <ul><li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFHesselsRansomStairsFreire2003" class="citation journal cs1">Hessels, Jason W. T; Ransom, Scott M; Stairs, Ingrid H; Freire, Paulo C. C; Kaspi, Victoria M; Camilo, Fernando (2003). "Neutron Stars for Undergraduates". <i>American Journal of Physics</i>. <b>72</b> (2004): <span class="nowrap">892–</span>905. <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<span class="id-lock-free" title="Freely accessible"><a rel="nofollow" class="external text" href="https://arxiv.org/abs/nucl-th/0309041">nucl-th/0309041</a></span>. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2004AmJPh..72..892S">2004AmJPh..72..892S</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1119%2F1.1703544">10.1119/1.1703544</a>. <a href="/wiki/S2CID_(identifier)" class="mw-redirect" title="S2CID (identifier)">S2CID</a> <a rel="nofollow" class="external text" href="https://api.semanticscholar.org/CorpusID:27807404">27807404</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=American+Journal+of+Physics&rft.atitle=Neutron+Stars+for+Undergraduates&rft.volume=72&rft.issue=2004&rft.pages=%3Cspan+class%3D%22nowrap%22%3E892-%3C%2Fspan%3E905&rft.date=2003&rft_id=info%3Aarxiv%2Fnucl-th%2F0309041&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A27807404%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.1119%2F1.1703544&rft_id=info%3Abibcode%2F2004AmJPh..72..892S&rft.aulast=Hessels&rft.aufirst=Jason+W.+T&rft.au=Ransom%2C+Scott+M&rft.au=Stairs%2C+Ingrid+H&rft.au=Freire%2C+Paulo+C.+C&rft.au=Kaspi%2C+Victoria+M&rft.au=Camilo%2C+Fernando&rfr_id=info%3Asid%2Fen.wikipedia.org%3ANeutron+star" class="Z3988"></span> <ul><li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFSilbarReddy2005" class="citation journal cs1">Silbar, Richard R; Reddy, Sanjay (2005). "Erratum: "Neutron stars for undergraduates" [Am. J. Phys. 72 (7), 892–905 (2004)]". <i>American Journal of Physics</i>. <b>73</b> (3): 286. <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<span class="id-lock-free" title="Freely accessible"><a rel="nofollow" class="external text" href="https://arxiv.org/abs/nucl-th/0309041">nucl-th/0309041</a></span>. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2005AmJPh..73..286S">2005AmJPh..73..286S</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1119%2F1.1852544">10.1119/1.1852544</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=American+Journal+of+Physics&rft.atitle=Erratum%3A+%22Neutron+stars+for+undergraduates%22+%26%2391%3BAm.+J.+Phys.+72+%287%29%2C+892%E2%80%93905+%282004%29%26%2393%3B&rft.volume=73&rft.issue=3&rft.pages=286&rft.date=2005&rft_id=info%3Aarxiv%2Fnucl-th%2F0309041&rft_id=info%3Adoi%2F10.1119%2F1.1852544&rft_id=info%3Abibcode%2F2005AmJPh..73..286S&rft.aulast=Silbar&rft.aufirst=Richard+R&rft.au=Reddy%2C+Sanjay&rfr_id=info%3Asid%2Fen.wikipedia.org%3ANeutron+star" class="Z3988"></span></li></ul></li> <li><a rel="nofollow" class="external text" href="https://web.archive.org/web/20090326222943/https://imagine.gsfc.nasa.gov/docs/science/know_l2/pulsars.html">NASA on pulsars</a></li> <li>"<a rel="nofollow" class="external text" href="https://www.spacedaily.com/reports/NASA_Sees_Hidden_Structure_Of_Neutron_Star_In_Starquake.html">NASA Sees Hidden Structure Of Neutron Star In Starquake</a>". SpaceDaily.com. April 26, 2006</li> <li>"<a rel="nofollow" class="external text" href="https://www.newscientist.com/article/dn9397-mysterious-x-ray-sources-may-be-lone-neutron-stars/">Mysterious X-ray sources may be lone neutron stars</a>" David Shiga. <i>New Scientist</i>. 23 June 2006</li> <li>"<a rel="nofollow" class="external text" href="https://www.newscientist.com/article/dn9428-massive-neutron-star-rules-out-exotic-matter/">Massive neutron star rules out exotic matter</a>". <i>New Scientist</i>. According to a new analysis, exotic states of matter such as free quarks or BECs do not arise inside neutron stars.</li> <li>"<a rel="nofollow" class="external text" href="https://www.newscientist.com/article/dn9730-neutron-star-clocked-at-mind-boggling-velocity">Neutron star clocked at mind-boggling velocity</a>". <i>New Scientist</i>. A neutron star has been clocked traveling at more than 1500 kilometers per second.</li></ul> <div class="navbox-styles"><style data-mw-deduplicate="TemplateStyles:r1129693374">.mw-parser-output .hlist dl,.mw-parser-output .hlist ol,.mw-parser-output .hlist ul{margin:0;padding:0}.mw-parser-output .hlist dd,.mw-parser-output .hlist dt,.mw-parser-output .hlist li{margin:0;display:inline}.mw-parser-output .hlist.inline,.mw-parser-output .hlist.inline dl,.mw-parser-output .hlist.inline ol,.mw-parser-output .hlist.inline ul,.mw-parser-output .hlist dl dl,.mw-parser-output .hlist dl ol,.mw-parser-output .hlist dl ul,.mw-parser-output .hlist ol dl,.mw-parser-output .hlist ol ol,.mw-parser-output .hlist ol ul,.mw-parser-output .hlist ul dl,.mw-parser-output .hlist ul ol,.mw-parser-output .hlist ul ul{display:inline}.mw-parser-output .hlist .mw-empty-li{display:none}.mw-parser-output .hlist dt::after{content:": "}.mw-parser-output .hlist dd::after,.mw-parser-output .hlist li::after{content:" · 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abbr{color:var(--color-base)!important}@media(prefers-color-scheme:dark){html.skin-theme-clientpref-os .mw-parser-output .navbar li a abbr{color:var(--color-base)!important}}@media print{.mw-parser-output .navbar{display:none!important}}</style><div class="navbar plainlinks hlist navbar-mini"><ul><li class="nv-view"><a href="/wiki/Template:Neutron_star" title="Template:Neutron star"><abbr title="View this template">v</abbr></a></li><li class="nv-talk"><a href="/wiki/Template_talk:Neutron_star" title="Template talk:Neutron star"><abbr title="Discuss this template">t</abbr></a></li><li class="nv-edit"><a href="/wiki/Special:EditPage/Template:Neutron_star" title="Special:EditPage/Template:Neutron star"><abbr title="Edit this template">e</abbr></a></li></ul></div><div id="Neutron_star343" style="font-size:114%;margin:0 4em"><a class="mw-selflink selflink">Neutron star</a></div></th></tr><tr><th scope="row" class="navbox-group" style="width:1%">Types</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Radio-quiet_neutron_star" title="Radio-quiet neutron star">Radio-quiet</a></li> <li><a href="/wiki/Pulsar" title="Pulsar">Pulsar</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Single pulsars</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Magnetar" title="Magnetar">Magnetar</a> <ul><li><a href="/wiki/Soft_gamma_repeater" title="Soft gamma repeater">Soft gamma repeater</a></li> <li><a href="/wiki/Anomalous_X-ray_pulsar" title="Anomalous X-ray pulsar">Anomalous X-ray</a></li> <li>Ultra-long period</li></ul></li> <li><a href="/wiki/Rotating_radio_transient" title="Rotating radio transient">Rotating radio transient</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Binary pulsars</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Binary_pulsar" title="Binary pulsar">Binary</a></li> <li><a href="/wiki/X-ray_pulsar" title="X-ray pulsar">X-ray pulsar</a> <ul><li><a href="/wiki/X-ray_binary" title="X-ray binary">X-ray binary</a></li> <li><a href="/wiki/X-ray_burster" title="X-ray burster">X-ray burster</a></li> <li><a href="/wiki/List_of_X-ray_pulsars" title="List of X-ray pulsars">List</a></li></ul></li> <li><a href="/wiki/Millisecond_pulsar" title="Millisecond pulsar">Millisecond</a></li> <li><a href="/wiki/Be/X-ray_binary" title="Be/X-ray binary">Be/X-ray</a></li> <li><a href="/wiki/Neutron_star_spin-up" title="Neutron star spin-up">Spin-up</a></li> <li><a href="/wiki/Hulse%E2%80%93Taylor_pulsar" title="Hulse–Taylor pulsar">Hulse–Taylor pulsar</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Properties</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Blitzar" title="Blitzar">Blitzar</a> <ul><li><a href="/wiki/Fast_radio_burst" title="Fast radio burst">Fast radio burst</a></li></ul></li> <li><a href="/wiki/Bondi_accretion" title="Bondi accretion">Bondi accretion</a></li> <li><a href="/wiki/Chandrasekhar_limit" title="Chandrasekhar limit">Chandrasekhar limit</a></li> <li><a href="/wiki/Gamma-ray_burst" title="Gamma-ray burst">Gamma-ray burst</a></li> <li><a href="/wiki/Glitch_(astronomy)" title="Glitch (astronomy)">Glitch</a></li> <li><a href="/wiki/Neutron_matter" class="mw-redirect" title="Neutron matter">Neutron matter</a></li> <li><a href="/wiki/Neutron-star_oscillation" title="Neutron-star oscillation">Neutron-star oscillation</a></li> <li><a href="/wiki/Optical_pulsar" title="Optical pulsar">Optical</a></li> <li><a href="/wiki/Pulsar_kick" title="Pulsar kick">Pulsar kick</a></li> <li><a href="/wiki/Quasi-periodic_oscillation" class="mw-redirect" title="Quasi-periodic oscillation">Quasi-periodic oscillation</a></li> <li><a href="/wiki/Relativistic_star" title="Relativistic star">Relativistic</a></li> <li><a href="/wiki/Rp-process" title="Rp-process">Rp-process</a></li> <li><a href="/wiki/Starquake_(astrophysics)" class="mw-redirect" title="Starquake (astrophysics)">Starquake</a></li> <li><a href="/wiki/Pulsar#Precise_clocks" title="Pulsar">Timing noise</a></li> <li><a href="/wiki/Tolman%E2%80%93Oppenheimer%E2%80%93Volkoff_limit" title="Tolman–Oppenheimer–Volkoff limit">Tolman–Oppenheimer–Volkoff limit</a></li> <li><a href="/wiki/Urca_process" title="Urca process">Urca process</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Related</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Gamma-ray_burst_progenitors" title="Gamma-ray burst progenitors">Gamma-ray burst progenitors</a></li> <li><a href="/wiki/Asteroseismology" title="Asteroseismology">Asteroseismology</a></li> <li><a href="/wiki/Compact_star" class="mw-redirect" title="Compact star">Compact star</a> <ul><li><a href="/wiki/Quark_star" title="Quark star">Quark star</a></li> <li><a href="/wiki/Exotic_star" title="Exotic star">Exotic star</a></li></ul></li> <li><a href="/wiki/Supernova" title="Supernova">Supernova</a> <ul><li><a href="/wiki/Supernova_remnant" title="Supernova remnant">Supernova remnant</a></li> <li><a href="/wiki/Template:Supernovae" title="Template:Supernovae">Related links</a></li></ul></li> <li><a href="/wiki/Hypernova" title="Hypernova">Hypernova</a></li> <li><a href="/wiki/Kilonova" title="Kilonova">Kilonova</a></li> <li><a href="/wiki/Microquasar" title="Microquasar">Microquasar</a></li> <li><a href="/wiki/Neutron_star_merger" title="Neutron star merger">Neutron star merger</a></li> <li><a href="/wiki/Quark-nova" title="Quark-nova">Quark-nova</a></li> <li><a href="/wiki/White_dwarf" title="White dwarf">White dwarf</a> <ul><li><a href="/wiki/Template:White_dwarf" title="Template:White dwarf">Related links</a></li></ul></li> <li><a href="/wiki/Stellar_black_hole" title="Stellar black hole">Stellar black hole</a> <ul><li><a href="/wiki/Template:Black_holes" title="Template:Black holes">Related links</a></li></ul></li> <li><a href="/wiki/Radio_star" title="Radio star">Radio star</a></li> <li><a href="/wiki/Pulsar_planet" title="Pulsar planet">Pulsar planet</a></li> <li><a href="/wiki/Pulsar_wind_nebula" title="Pulsar wind nebula">Pulsar wind nebula</a></li> <li><a href="/wiki/Thorne%E2%80%93%C5%BBytkow_object" title="Thorne–Żytkow object">Thorne–Żytkow object</a></li> <li><a href="/wiki/QCD_matter" title="QCD matter">QCD matter</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Discovery</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/PSR_B1919%2B21" title="PSR B1919+21">LGM-1</a></li> <li><a href="/wiki/Centaurus_X-3" title="Centaurus X-3">Centaurus X-3</a></li> <li><a href="/wiki/Timeline_of_white_dwarfs,_neutron_stars,_and_supernovae" title="Timeline of white dwarfs, neutron stars, and supernovae">Timeline of white dwarfs, neutron stars, and supernovae</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Satellite<br />investigation</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Rossi_X-ray_Timing_Explorer" title="Rossi X-ray Timing Explorer">Rossi X-ray Timing Explorer</a></li> <li><a href="/wiki/Fermi_Gamma-ray_Space_Telescope" title="Fermi Gamma-ray Space Telescope">Fermi Gamma-ray Space Telescope</a></li> <li><a href="/wiki/Compton_Gamma_Ray_Observatory" title="Compton Gamma Ray Observatory">Compton Gamma Ray Observatory</a></li> <li><a href="/wiki/Chandra_X-ray_Observatory" title="Chandra X-ray Observatory">Chandra X-ray Observatory</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Other</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/X-ray_pulsar-based_navigation" class="mw-redirect" title="X-ray pulsar-based navigation">X-ray pulsar-based navigation</a></li> <li><a href="/wiki/The_Magnificent_Seven_(neutron_stars)" title="The Magnificent Seven (neutron stars)">The Magnificent Seven</a></li> <li><a href="/wiki/List_of_neutron_stars" title="List of neutron stars">List of neutron stars</a> <ul><li><a href="/wiki/List_of_most_massive_neutron_stars" title="List of most massive neutron stars">Most massive neutron stars</a></li></ul></li> <li><a href="/wiki/Neutron_stars_in_fiction" title="Neutron stars in fiction">Neutron stars in fiction</a></li></ul> </div></td></tr><tr><td class="navbox-abovebelow" colspan="2"><div> <ul><li><span class="noviewer" typeof="mw:File"><span title="Category"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/16px-Symbol_category_class.svg.png" decoding="async" width="16" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/23px-Symbol_category_class.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/31px-Symbol_category_class.svg.png 2x" data-file-width="180" data-file-height="185" /></span></span> <a href="/wiki/Category:Neutron_stars" title="Category:Neutron stars">Category</a></li> <li><span class="noviewer" typeof="mw:File"><span title="Commons page"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/4/4a/Commons-logo.svg/12px-Commons-logo.svg.png" decoding="async" width="12" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/4/4a/Commons-logo.svg/18px-Commons-logo.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/4/4a/Commons-logo.svg/24px-Commons-logo.svg.png 2x" data-file-width="1024" data-file-height="1376" /></span></span> <a href="https://commons.wikimedia.org/wiki/Category:Neutron_stars" class="extiw" title="commons:Category:Neutron stars">Commons</a></li></ul> </div></td></tr></tbody></table></div> <div class="navbox-styles"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1129693374"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236075235"></div><div role="navigation" class="navbox" aria-labelledby="White_dwarf298" style="padding:3px"><table class="nowraplinks hlist mw-collapsible autocollapse navbox-inner" style="border-spacing:0;background:transparent;color:inherit"><tbody><tr><th scope="col" class="navbox-title" colspan="2"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1129693374"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1239400231"><div class="navbar plainlinks hlist navbar-mini"><ul><li class="nv-view"><a href="/wiki/Template:White_dwarf" title="Template:White dwarf"><abbr title="View this template">v</abbr></a></li><li class="nv-talk"><a href="/wiki/Template_talk:White_dwarf" title="Template talk:White dwarf"><abbr title="Discuss this template">t</abbr></a></li><li class="nv-edit"><a href="/wiki/Special:EditPage/Template:White_dwarf" title="Special:EditPage/Template:White dwarf"><abbr title="Edit this template">e</abbr></a></li></ul></div><div id="White_dwarf298" style="font-size:114%;margin:0 4em"><a href="/wiki/White_dwarf" title="White dwarf">White dwarf</a></div></th></tr><tr><th scope="row" class="navbox-group" style="width:1%">Formation</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Chandrasekhar_limit" title="Chandrasekhar limit">Chandrasekhar limit</a></li> <li><a href="/wiki/Hertzsprung%E2%80%93Russell_diagram" title="Hertzsprung–Russell diagram">Hertzsprung–Russell diagram</a></li> <li><a href="/wiki/Mira_variable" title="Mira variable">Mira variable</a></li> <li><a href="/wiki/PG_1159_star" title="PG 1159 star">PG 1159 star</a></li> <li><a href="/wiki/Stellar_evolution" title="Stellar evolution">Stellar evolution</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Fate</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Black_dwarf" title="Black dwarf">Black dwarf</a></li> <li><a href="/wiki/Type_Ia_supernova" title="Type Ia supernova">Type Ia supernova</a> <ul><li><a href="/wiki/List_of_supernova_candidates" title="List of supernova candidates">Candidates</a></li></ul></li> <li><a class="mw-selflink selflink">Neutron star</a> <ul><li><a href="/wiki/Pulsar" title="Pulsar">Pulsar</a></li> <li><a href="/wiki/Magnetar" title="Magnetar">Magnetar</a></li> <li><a href="/wiki/Template:Neutron_star" title="Template:Neutron star">Related links</a></li></ul></li> <li><a href="/wiki/Stellar_black_hole" title="Stellar black hole">Stellar black hole</a> <ul><li><a href="/wiki/Template:Black_holes" title="Template:Black holes">Related links</a></li></ul></li> <li><a href="/wiki/Compact_star" class="mw-redirect" title="Compact star">Compact star</a> <ul><li><a href="/wiki/Quark_star" title="Quark star">Quark star</a></li> <li><a href="/wiki/Exotic_star" title="Exotic star">Exotic star</a></li></ul></li> <li><a href="/wiki/Extreme_helium_star" title="Extreme helium star">Extreme helium star</a></li> <li><a href="/wiki/Subdwarf_B_star" title="Subdwarf B star">Subdwarf B star</a></li> <li><a href="/wiki/Helium_planet" title="Helium planet">Helium planet</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">In binary<br />systems</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Nova" title="Nova">Nova</a> <ul><li><a href="/wiki/Nova_remnant" title="Nova remnant">Remnant</a></li> <li><a href="/wiki/List_of_novae" class="mw-redirect" title="List of novae">List</a></li></ul></li> <li><a href="/wiki/Dwarf_nova" title="Dwarf nova">Dwarf nova</a></li> <li><a href="/wiki/Micronova" title="Micronova">Micronova</a></li> <li><a href="/wiki/Symbiotic_nova" title="Symbiotic nova">Symbiotic nova</a></li> <li><a href="/wiki/Cataclysmic_variable_star" title="Cataclysmic variable star">Cataclysmic variable star</a> <ul><li><a href="/wiki/AM_CVn_star" class="mw-redirect" title="AM CVn star">AM CVn star</a></li> <li><a href="/wiki/Polar_(cataclysmic_variable)" class="mw-redirect" title="Polar (cataclysmic variable)">Polar</a></li> <li><a href="/wiki/Intermediate_polar" title="Intermediate polar">Intermediate polar</a></li></ul></li> <li><a href="/wiki/X-ray_binary" title="X-ray binary">X-ray binary</a> <ul><li><a href="/wiki/Super_soft_X-ray_source" title="Super soft X-ray source">Super soft X-ray source</a></li></ul></li> <li><a href="/wiki/Binary_pulsar" title="Binary pulsar">Binary pulsar</a></li> <li><a href="/wiki/Helium_flash" title="Helium flash">Helium flash</a></li> <li><a href="/wiki/Carbon_detonation" title="Carbon detonation">Carbon detonation</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Properties</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Pulsating_white_dwarf" title="Pulsating white dwarf">Pulsating</a></li> <li><a href="/wiki/Urca_process" title="Urca process">Urca process</a></li> <li><a href="/wiki/Degenerate_matter#Electron_degeneracy" title="Degenerate matter">Electron-degenerate matter</a></li> <li><a href="/wiki/Quasi-periodic_oscillations" class="mw-redirect" title="Quasi-periodic oscillations">Quasi-periodic oscillations</a></li> <li><a href="/wiki/White_dwarf_cooling_anomaly" title="White dwarf cooling anomaly">White dwarf cooling anomaly</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Related</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Planetary_nebula" title="Planetary nebula">Planetary nebula</a> <ul><li><a href="/wiki/List_of_planetary_nebulae" title="List of planetary nebulae">List</a></li></ul></li> <li><a href="/wiki/Robust_associations_of_massive_baryonic_objects" title="Robust associations of massive baryonic objects">RAMBOs</a></li> <li><a href="/wiki/White_dwarf_luminosity_function" class="mw-redirect" title="White dwarf luminosity function">White dwarf luminosity function</a></li> <li><a href="/wiki/Timeline_of_white_dwarfs,_neutron_stars,_and_supernovae" title="Timeline of white dwarfs, neutron stars, and supernovae">Timeline of white dwarfs, neutron stars, and supernovae</a></li></ul> </div></td></tr><tr><td class="navbox-abovebelow" colspan="2"><div> <ul><li><span class="noviewer" typeof="mw:File"><span title="List-Class article"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/d/db/Symbol_list_class.svg/16px-Symbol_list_class.svg.png" decoding="async" width="16" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/d/db/Symbol_list_class.svg/23px-Symbol_list_class.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/d/db/Symbol_list_class.svg/31px-Symbol_list_class.svg.png 2x" data-file-width="180" data-file-height="185" /></span></span> <a href="/wiki/List_of_white_dwarfs" title="List of white dwarfs">List</a></li> <li><span class="noviewer" typeof="mw:File"><span title="Category"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/16px-Symbol_category_class.svg.png" decoding="async" width="16" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/23px-Symbol_category_class.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/31px-Symbol_category_class.svg.png 2x" data-file-width="180" data-file-height="185" /></span></span> <a href="/wiki/Category:White_dwarfs" title="Category:White dwarfs">Category</a></li></ul> </div></td></tr></tbody></table></div> <div class="navbox-styles"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1129693374"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236075235"></div><div role="navigation" class="navbox" aria-labelledby="Black_holes386" style="padding:3px"><table class="nowraplinks hlist mw-collapsible autocollapse navbox-inner" style="border-spacing:0;background:transparent;color:inherit"><tbody><tr><th scope="col" class="navbox-title" colspan="3" style="text-align:center;"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1129693374"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1239400231"><div class="navbar plainlinks hlist navbar-mini"><ul><li class="nv-view"><a href="/wiki/Template:Black_holes" title="Template:Black holes"><abbr title="View this template">v</abbr></a></li><li class="nv-talk"><a href="/wiki/Template_talk:Black_holes" title="Template talk:Black holes"><abbr title="Discuss this template">t</abbr></a></li><li class="nv-edit"><a href="/wiki/Special:EditPage/Template:Black_holes" title="Special:EditPage/Template:Black holes"><abbr title="Edit this template">e</abbr></a></li></ul></div><div id="Black_holes386" style="font-size:114%;margin:0 4em"><a href="/wiki/Black_hole" title="Black hole">Black holes</a></div></th></tr><tr><td class="navbox-abovebelow" colspan="3" style="text-align:center;"><div> <ul><li><a href="/wiki/Outline_of_black_holes" title="Outline of black holes">Outline</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="text-align:center;;width:1%">Types</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/BTZ_black_hole" title="BTZ black hole">BTZ black hole</a></li> <li><a href="/wiki/Schwarzschild_metric" title="Schwarzschild metric">Schwarzschild</a></li> <li><a href="/wiki/Rotating_black_hole" title="Rotating black hole">Rotating</a></li> <li><a href="/wiki/Charged_black_hole" title="Charged black hole">Charged</a></li> <li><a href="/wiki/Virtual_black_hole" title="Virtual black hole">Virtual</a></li> <li><a href="/wiki/Kugelblitz_(astrophysics)" title="Kugelblitz (astrophysics)">Kugelblitz</a></li> <li><a href="/wiki/Supermassive_black_hole" title="Supermassive black hole">Supermassive</a></li> <li><a href="/wiki/Primordial_black_hole" title="Primordial black hole">Primordial</a></li> <li><a href="/wiki/Direct_collapse_black_hole" title="Direct collapse black hole">Direct collapse</a></li> <li><a href="/wiki/Rogue_black_hole" title="Rogue black hole">Rogue</a></li> <li><a href="/wiki/Malament%E2%80%93Hogarth_spacetime" title="Malament–Hogarth spacetime">Malament–Hogarth spacetime</a></li></ul> </div></td><td class="noviewer navbox-image" rowspan="11" style="width:1px;padding:0 0 0 2px"><div><span typeof="mw:File"><a href="/wiki/File:Black_hole_-_Messier_87_crop_max_res.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/4/4f/Black_hole_-_Messier_87_crop_max_res.jpg/80px-Black_hole_-_Messier_87_crop_max_res.jpg" decoding="async" width="80" height="80" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/4/4f/Black_hole_-_Messier_87_crop_max_res.jpg/120px-Black_hole_-_Messier_87_crop_max_res.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/4/4f/Black_hole_-_Messier_87_crop_max_res.jpg/160px-Black_hole_-_Messier_87_crop_max_res.jpg 2x" data-file-width="4320" data-file-height="4320" /></a></span></div></td></tr><tr><th scope="row" class="navbox-group" style="text-align:center;;width:1%">Size</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Micro_black_hole" title="Micro black hole">Micro</a> <ul><li><a href="/wiki/Extremal_black_hole" title="Extremal black hole">Extremal</a></li> <li><a href="/wiki/Black_hole_electron" title="Black hole electron">Electron</a></li></ul></li> <li><a href="/wiki/Stellar_black_hole" title="Stellar black hole">Stellar</a> <ul><li><a href="/wiki/Microquasar" title="Microquasar">Microquasar</a></li></ul></li> <li><a href="/wiki/Intermediate-mass_black_hole" title="Intermediate-mass black hole">Intermediate-mass</a></li> <li><a href="/wiki/Supermassive_black_hole" title="Supermassive black hole">Supermassive</a> <ul><li><a href="/wiki/Active_galactic_nucleus" title="Active galactic nucleus">Active galactic nucleus</a></li> <li><a href="/wiki/Quasar" title="Quasar">Quasar</a></li> <li><a href="/wiki/Large_quasar_group" title="Large quasar group">LQG</a></li> <li><a href="/wiki/Blazar" title="Blazar">Blazar</a></li> <li><a href="/wiki/OVV_quasar" title="OVV quasar">OVV</a></li></ul></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="text-align:center;;width:1%">Formation</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Stellar_evolution" title="Stellar evolution">Stellar evolution</a></li> <li><a href="/wiki/Gravitational_collapse" title="Gravitational collapse">Gravitational collapse</a></li> <li><a class="mw-selflink selflink">Neutron star</a> <ul><li><a href="/wiki/Template:Neutron_star" title="Template:Neutron star">Related links</a></li></ul></li> <li><a href="/wiki/Tolman%E2%80%93Oppenheimer%E2%80%93Volkoff_limit" title="Tolman–Oppenheimer–Volkoff limit">Tolman–Oppenheimer–Volkoff limit</a></li> <li><a href="/wiki/White_dwarf" title="White dwarf">White dwarf</a> <ul><li><a href="/wiki/Template:White_dwarf" title="Template:White dwarf">Related links</a></li></ul></li> <li><a href="/wiki/Supernova" title="Supernova">Supernova</a> <ul><li><a href="/wiki/Micronova" title="Micronova">Micronova</a></li> <li><a href="/wiki/Superluminous_supernova" title="Superluminous supernova">Hypernova</a></li> <li><a href="/wiki/Template:Supernovae" title="Template:Supernovae">Related links</a></li></ul></li> <li><a href="/wiki/Gamma-ray_burst" title="Gamma-ray burst">Gamma-ray burst</a></li> <li><a href="/wiki/Binary_black_hole" title="Binary black hole">Binary black hole</a></li> <li><a href="/wiki/Quark_star" title="Quark star">Quark star</a></li> <li><a href="/wiki/Supermassive_star" class="mw-redirect" title="Supermassive star">Supermassive star</a></li> <li><a href="/wiki/Quasi-star" title="Quasi-star">Quasi-star</a></li> <li><a href="/wiki/Dark_star_(dark_matter)" title="Dark star (dark matter)">Supermassive dark star</a></li> <li><a href="/wiki/X-ray_binary" title="X-ray binary">X-ray binary</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="text-align:center;;width:1%">Properties</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Astrophysical_jet" title="Astrophysical jet">Astrophysical jet</a></li> <li><a href="/wiki/Gravitational_singularity" title="Gravitational singularity">Gravitational singularity</a> <ul><li><a href="/wiki/Ring_singularity" title="Ring singularity">Ring singularity</a></li> <li><a href="/wiki/Penrose%E2%80%93Hawking_singularity_theorems" title="Penrose–Hawking singularity theorems">Theorems</a></li></ul></li> <li><a href="/wiki/Event_horizon" title="Event horizon">Event horizon</a></li> <li><a href="/wiki/Photon_sphere" title="Photon sphere">Photon sphere</a></li> <li><a href="/wiki/Innermost_stable_circular_orbit" title="Innermost stable circular orbit">Innermost stable circular orbit</a></li> <li><a href="/wiki/Ergosphere" title="Ergosphere">Ergosphere</a> <ul><li><a href="/wiki/Penrose_process" title="Penrose process">Penrose process</a></li> <li><a href="/wiki/Blandford%E2%80%93Znajek_process" title="Blandford–Znajek process">Blandford–Znajek process</a></li></ul></li> <li><a href="/wiki/Accretion_disk" title="Accretion disk">Accretion disk</a></li> <li><a href="/wiki/Hawking_radiation" title="Hawking radiation">Hawking radiation</a></li> <li><a href="/wiki/Gravitational_lens" title="Gravitational lens">Gravitational lens</a> <ul><li><a href="/wiki/Gravitational_microlensing" title="Gravitational microlensing">Microlens</a></li></ul></li> <li><a href="/wiki/Bondi_accretion" title="Bondi accretion">Bondi accretion</a></li> <li><a href="/wiki/M%E2%80%93sigma_relation" title="M–sigma relation">M–sigma relation</a></li> <li><a href="/wiki/Quasi-periodic_oscillation" class="mw-redirect" title="Quasi-periodic oscillation">Quasi-periodic oscillation</a></li> <li><a href="/wiki/Black_hole_thermodynamics" title="Black hole thermodynamics">Thermodynamics</a></li> <li><a href="/wiki/Bekenstein_bound" title="Bekenstein bound">Bekenstein bound</a></li> <li><a href="/wiki/Bousso%27s_holographic_bound" title="Bousso's holographic bound">Bousso's holographic bound</a> <ul><li><a href="/wiki/Immirzi_parameter" title="Immirzi parameter">Immirzi parameter</a></li></ul></li> <li><a href="/wiki/Schwarzschild_radius" title="Schwarzschild radius">Schwarzschild radius</a></li> <li><a href="/wiki/Spaghettification" title="Spaghettification">Spaghettification</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="text-align:center;;width:1%">Issues</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Black_hole_complementarity" title="Black hole complementarity">Black hole complementarity</a></li> <li><a href="/wiki/Black_hole_information_paradox" title="Black hole information paradox">Information paradox</a></li> <li><a href="/wiki/Cosmic_censorship_hypothesis" title="Cosmic censorship hypothesis">Cosmic censorship</a></li> <li><a href="/wiki/ER_%3D_EPR" title="ER = EPR">ER = EPR</a></li> <li><a href="/wiki/Binary_black_hole#Final_parsec_problem" title="Binary black hole">Final parsec problem</a></li> <li><a href="/wiki/Firewall_(physics)" title="Firewall (physics)">Firewall (physics)</a></li> <li><a href="/wiki/Holographic_principle" title="Holographic principle">Holographic principle</a></li> <li><a href="/wiki/No-hair_theorem" title="No-hair theorem">No-hair theorem</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="text-align:center;;width:1%">Metrics</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Schwarzschild_metric" title="Schwarzschild metric">Schwarzschild</a> (<a href="/wiki/Derivation_of_the_Schwarzschild_solution" title="Derivation of the Schwarzschild solution">Derivation</a>)</li> <li><a href="/wiki/Kerr_metric" title="Kerr metric">Kerr</a></li> <li><a href="/wiki/Reissner%E2%80%93Nordstr%C3%B6m_metric" title="Reissner–Nordström metric">Reissner–Nordström</a></li> <li><a href="/wiki/Kerr%E2%80%93Newman_metric" title="Kerr–Newman metric">Kerr–Newman</a></li> <li><a href="/wiki/Hayward_metric" title="Hayward metric">Hayward</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="text-align:center;;width:1%">Alternatives</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Nonsingular_black_hole_models" title="Nonsingular black hole models">Nonsingular black hole models</a></li> <li><a href="/wiki/Black_star_(semiclassical_gravity)" title="Black star (semiclassical gravity)">Black star</a></li> <li><a href="/wiki/Dark_star_(Newtonian_mechanics)" title="Dark star (Newtonian mechanics)">Dark star</a></li> <li><a href="/wiki/Dark-energy_star" title="Dark-energy star">Dark-energy star</a></li> <li><a href="/wiki/Gravastar" title="Gravastar">Gravastar</a></li> <li><a href="/wiki/Magnetospheric_eternally_collapsing_object" title="Magnetospheric eternally collapsing object">Magnetospheric eternally collapsing object</a></li> <li><a href="/wiki/Planck_star" title="Planck star">Planck star</a></li> <li><a href="/wiki/Q_star" title="Q star">Q star</a></li> <li><a href="/wiki/Fuzzball_(string_theory)" title="Fuzzball (string theory)">Fuzzball</a></li> <li><a href="/wiki/Geon_(physics)" title="Geon (physics)">Geon</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="text-align:center;;width:1%">Analogs</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Optical_black_hole" title="Optical black hole">Optical black hole</a></li> <li><a href="/wiki/Sonic_black_hole" title="Sonic black hole">Sonic black hole</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="text-align:center;;width:1%"><a href="/wiki/Lists_of_black_holes" title="Lists of black holes">Lists</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/List_of_black_holes" title="List of black holes">Black holes</a></li> <li><a href="/wiki/List_of_most_massive_black_holes" title="List of most massive black holes">Most massive</a></li> <li><a href="/wiki/List_of_nearest_known_black_holes" title="List of nearest known black holes">Nearest</a></li> <li><a href="/wiki/List_of_quasars" title="List of quasars">Quasars</a></li> <li><a href="/wiki/List_of_microquasars" title="List of microquasars">Microquasars</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="text-align:center;;width:1%">Related</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Outline_of_black_holes" title="Outline of black holes">Outline of black holes</a></li> <li><a href="/wiki/Black_Hole_Initiative" title="Black Hole Initiative">Black Hole Initiative</a></li> <li><a href="/wiki/Black_hole_starship" title="Black hole starship">Black hole starship</a></li> <li><a href="/wiki/Black_holes_in_fiction" title="Black holes in fiction">Black holes in fiction</a></li> <li><a href="/wiki/Big_Bang" title="Big Bang">Big Bang</a></li> <li><a href="/wiki/Big_Bounce" title="Big Bounce">Big Bounce</a></li> <li><a href="/wiki/Compact_star" class="mw-redirect" title="Compact star">Compact star</a></li> <li><a href="/wiki/Exotic_star" title="Exotic star">Exotic star</a> <ul><li><a href="/wiki/Quark_star" title="Quark star">Quark star</a></li> <li><a href="/wiki/Preon_star" class="mw-redirect" title="Preon star">Preon star</a></li></ul></li> <li><a href="/wiki/Gravitational_waves" class="mw-redirect" title="Gravitational waves">Gravitational waves</a></li> <li><a href="/wiki/Gamma-ray_burst_progenitors" title="Gamma-ray burst progenitors">Gamma-ray burst progenitors</a></li> <li><a href="/wiki/Gravity_well" class="mw-redirect" title="Gravity well">Gravity well</a></li> <li><a href="/wiki/Hypercompact_stellar_system" title="Hypercompact stellar system">Hypercompact stellar system</a></li> <li><a href="/wiki/Membrane_paradigm" title="Membrane paradigm">Membrane paradigm</a></li> <li><a href="/wiki/Naked_singularity" title="Naked singularity">Naked singularity</a></li> <li><a href="/wiki/Population_III_star" class="mw-redirect" title="Population III star">Population III star</a></li> <li><a href="/wiki/Supermassive_star" class="mw-redirect" title="Supermassive star">Supermassive star</a></li> <li><a href="/wiki/Quasi-star" title="Quasi-star">Quasi-star</a></li> <li><a href="/wiki/Dark_star_(dark_matter)" title="Dark star (dark matter)">Supermassive dark star</a></li> <li><a href="/wiki/Rossi_X-ray_Timing_Explorer" title="Rossi X-ray Timing Explorer">Rossi X-ray Timing Explorer</a></li> <li><a href="/wiki/Superluminal_motion" title="Superluminal motion">Superluminal motion</a></li> <li><a href="/wiki/Timeline_of_black_hole_physics" title="Timeline of black hole physics">Timeline of black hole physics</a></li> <li><a href="/wiki/White_hole" title="White hole">White hole</a></li> <li><a href="/wiki/Wormhole" title="Wormhole">Wormhole</a></li> <li><a href="/wiki/Tidal_disruption_event" title="Tidal disruption event">Tidal disruption event</a></li> <li><a href="/wiki/Planet_Nine" title="Planet Nine">Planet Nine</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="text-align:center;;width:1%">Notable</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Cygnus_X-1" title="Cygnus X-1">Cygnus X-1</a></li> <li><a href="/wiki/XTE_J1650-500" class="mw-redirect" title="XTE J1650-500">XTE J1650-500</a></li> <li><a href="/wiki/XTE_J1118%2B480" title="XTE J1118+480">XTE J1118+480</a></li> <li><a href="/wiki/A0620-00" title="A0620-00">A0620-00</a></li> <li><a href="/wiki/Sagittarius_A*" title="Sagittarius A*">Sagittarius A*</a></li> <li><a href="/wiki/Centaurus_A" title="Centaurus A">Centaurus A</a></li> <li><a href="/wiki/Phoenix_Cluster" title="Phoenix Cluster">Phoenix Cluster</a></li> <li><a href="/wiki/PKS_1302-102" class="mw-redirect" title="PKS 1302-102">PKS 1302-102</a></li> <li><a href="/wiki/OJ_287" title="OJ 287">OJ 287</a></li> <li><a href="/wiki/SDSS_J0849%2B1114" title="SDSS J0849+1114">SDSS J0849+1114</a></li> <li><a href="/wiki/TON_618" title="TON 618">TON 618</a></li> <li><a href="/wiki/MS_0735.6%2B7421" title="MS 0735.6+7421">MS 0735.6+7421</a></li> <li><a href="/wiki/NeVe_1" title="NeVe 1">NeVe 1</a></li> <li><a href="/wiki/Hercules_A" title="Hercules A">Hercules A</a></li> <li><a href="/wiki/3C_273" title="3C 273">3C 273</a></li> <li><a href="/wiki/Q0906%2B6930" title="Q0906+6930">Q0906+6930</a></li> <li><a href="/wiki/Markarian_501" title="Markarian 501">Markarian 501</a></li> <li><a href="/wiki/ULAS_J1342%2B0928" title="ULAS J1342+0928">ULAS J1342+0928</a></li> <li><a href="/wiki/PSO_J030947.49%2B271757.31" title="PSO J030947.49+271757.31">PSO J030947.49+271757.31</a></li> <li><a href="/wiki/AT2018hyz" title="AT2018hyz">AT2018hyz</a></li> <li><a href="/wiki/Swift_J1644%2B57" title="Swift J1644+57">Swift J1644+57</a></li> <li><a href="/wiki/1ES_1927%2B654" title="1ES 1927+654">1ES 1927+654</a></li></ul> </div></td></tr><tr><td class="navbox-abovebelow hlist" colspan="3" style="text-align:center;"><div> <ul><li><span class="noviewer" typeof="mw:File"><span title="Category"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/16px-Symbol_category_class.svg.png" decoding="async" width="16" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/23px-Symbol_category_class.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/31px-Symbol_category_class.svg.png 2x" data-file-width="180" data-file-height="185" /></span></span> <a href="/wiki/Category:Black_holes" title="Category:Black holes">Category</a></li> <li><span class="noviewer" typeof="mw:File"><span title="Commons page"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/4/4a/Commons-logo.svg/12px-Commons-logo.svg.png" decoding="async" width="12" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/4/4a/Commons-logo.svg/18px-Commons-logo.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/4/4a/Commons-logo.svg/24px-Commons-logo.svg.png 2x" data-file-width="1024" data-file-height="1376" /></span></span> <a href="https://commons.wikimedia.org/wiki/Category:Black_holes" class="extiw" title="commons:Category:Black holes">Commons</a></li></ul> </div></td></tr></tbody></table></div> <div class="navbox-styles"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1129693374"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236075235"></div><div role="navigation" class="navbox" aria-labelledby="Stellar_core_collapse373" style="padding:3px"><table class="nowraplinks mw-collapsible autocollapse navbox-inner" style="border-spacing:0;background:transparent;color:inherit"><tbody><tr><th scope="col" class="navbox-title" colspan="3"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1129693374"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1239400231"><div class="navbar plainlinks hlist navbar-mini"><ul><li class="nv-view"><a href="/wiki/Template:Stellar_core_collapse" title="Template:Stellar core collapse"><abbr title="View this template">v</abbr></a></li><li class="nv-talk"><a href="/wiki/Template_talk:Stellar_core_collapse" title="Template talk:Stellar core collapse"><abbr title="Discuss this template">t</abbr></a></li><li class="nv-edit"><a href="/wiki/Special:EditPage/Template:Stellar_core_collapse" title="Special:EditPage/Template:Stellar core collapse"><abbr title="Edit this template">e</abbr></a></li></ul></div><div id="Stellar_core_collapse373" style="font-size:114%;margin:0 4em"><a href="/wiki/Stellar_core" title="Stellar core">Stellar core</a> <a href="/wiki/Gravitational_collapse" title="Gravitational collapse">collapse</a></div></th></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Star" title="Star">Stars</a></th><td class="navbox-list-with-group navbox-list navbox-odd hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Star_formation" title="Star formation">Formation</a></li> <li><a href="/wiki/Stellar_evolution" title="Stellar evolution">Evolution</a></li> <li><a href="/wiki/Stellar_structure" title="Stellar structure">Structure</a></li> <li><a href="/wiki/Stellar_core" title="Stellar core">Core</a></li> <li><a href="/wiki/Metallicity" title="Metallicity">Metallicity</a></li> <li><a href="/wiki/Stellar_physics" class="mw-redirect" title="Stellar physics">Stellar physics</a></li> <li><a href="/wiki/Astrophysical_plasma" title="Astrophysical plasma">Stellar plasma</a></li> <li><a href="/wiki/Supergiant_star" class="mw-redirect" title="Supergiant star">Supergiant</a></li> <li><a href="/wiki/Template:Variable_star_topics" title="Template:Variable star topics">Variable star</a></li> <li><a href="/wiki/Cataclysmic_variable_star" title="Cataclysmic variable star">Cataclysmic variable star</a></li> <li><a href="/wiki/Binary_star" title="Binary star">Binary star</a> <ul><li><a href="/wiki/X-ray_binary" title="X-ray binary">X-ray binary</a></li> <li><a href="/wiki/Super_soft_X-ray_source" title="Super soft X-ray source">Super soft X-ray source</a></li></ul></li></ul> </div></td><td class="noviewer navbox-image" rowspan="9" style="width:1px;padding:0 0 0 2px"><div><span typeof="mw:File"><a href="/wiki/File:Core_collapse_scenario.svg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/0/0c/Core_collapse_scenario.svg/270px-Core_collapse_scenario.svg.png" decoding="async" width="270" height="205" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/0/0c/Core_collapse_scenario.svg/405px-Core_collapse_scenario.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/0/0c/Core_collapse_scenario.svg/540px-Core_collapse_scenario.svg.png 2x" data-file-width="775" data-file-height="588" /></a></span></div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Stellar processes</th><td class="navbox-list-with-group navbox-list navbox-even hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Nuclear_fusion" title="Nuclear fusion">Nuclear fusion</a></li> <li><a href="/wiki/Nova" title="Nova">Surface fusion</a></li> <li><a href="/wiki/Stellar_nucleosynthesis" title="Stellar nucleosynthesis">Nucleosynthesis</a> <ul><li><a href="/wiki/R-process" title="R-process">R-process</a></li> <li><a href="/wiki/Rp-process" title="Rp-process">RP-process</a></li> <li><a href="/wiki/Supernova_nucleosynthesis" title="Supernova nucleosynthesis">Supernova nucleosynthesis</a></li></ul></li> <li><a href="/wiki/Accretion_(astrophysics)" title="Accretion (astrophysics)">Accretion</a> (<a href="/wiki/Bondi_accretion" title="Bondi accretion">Bondi accretion</a>)</li> <li><a href="/wiki/Electron_capture" title="Electron capture">Electron capture</a></li> <li><a href="/wiki/Carbon_detonation" title="Carbon detonation">Carbon detonation</a> / <a href="/wiki/Carbon_deflagration" class="mw-redirect" title="Carbon deflagration">deflagration</a></li> <li><a href="/wiki/Gamma-ray_burst" title="Gamma-ray burst">Gamma-ray burst</a></li> <li><a href="/wiki/Helium_flash" title="Helium flash">Helium flash</a></li> <li><a href="/wiki/Orbital_decay" title="Orbital decay">Orbital decay</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Collapse</th><td class="navbox-list-with-group navbox-list navbox-odd hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Gravitational_collapse" title="Gravitational collapse">Gravitational collapse</a></li> <li><a href="/wiki/Chandrasekhar_limit" title="Chandrasekhar limit">Chandrasekhar limit</a></li> <li><a href="/wiki/Tolman%E2%80%93Oppenheimer%E2%80%93Volkoff_limit" title="Tolman–Oppenheimer–Volkoff limit">Tolman–Oppenheimer–Volkoff limit</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Supernova" title="Supernova">Supernovae</a></th><td class="navbox-list-with-group navbox-list navbox-even hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Type_Ia_supernova" title="Type Ia supernova">Type Ia</a></li> <li><a href="/wiki/Type_Ib_and_Ic_supernovae" title="Type Ib and Ic supernovae">Type Ib and Ic</a></li> <li><a href="/wiki/Type_II_supernova" title="Type II supernova">Type II</a></li> <li><a href="/wiki/Pair-instability_supernova" title="Pair-instability supernova">Pair instability</a></li> <li><a href="/wiki/Hypernova" title="Hypernova">Hypernova</a></li> <li><a href="/wiki/Quark-nova" title="Quark-nova">Quark-nova</a></li> <li><a href="/wiki/Nebula" title="Nebula">Nebula</a></li> <li><a href="/wiki/Supernova_remnant" title="Supernova remnant">Remnant</a></li> <li><b><a href="/wiki/Template:Supernovae" title="Template:Supernovae">More...</a></b></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Compact_star" class="mw-redirect" title="Compact star">Compact and <br />exotic objects</a></th><td class="navbox-list-with-group navbox-list navbox-odd hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a class="mw-selflink selflink">Neutron star</a> <ul><li><a href="/wiki/Pulsar" title="Pulsar">Pulsar</a></li> <li><a href="/wiki/Quasar" title="Quasar">Quasar</a></li> <li><a href="/wiki/Magnetar" title="Magnetar">Magnetar</a></li> <li><a href="/wiki/Radio-quiet_neutron_star" title="Radio-quiet neutron star">Radio-quiet</a></li></ul></li> <li><a href="/wiki/White_dwarf" title="White dwarf">White dwarf</a></li> <li><a href="/wiki/Stellar_black_hole" title="Stellar black hole">Black hole</a></li> <li><a href="/wiki/Collapsar" title="Collapsar">Collapsar</a> <ul><li><a href="/wiki/Shell_collapsar" title="Shell collapsar">Shell collapsar</a></li></ul></li> <li><a href="/wiki/Exotic_star" title="Exotic star">Exotic star</a></li> <li><a href="/wiki/Quark_star" title="Quark star">Quark star</a></li> <li><a href="/wiki/Electroweak_star" class="mw-redirect" title="Electroweak star">Electroweak star</a></li> <li><a href="/wiki/Timeline_of_white_dwarfs,_neutron_stars,_and_supernovae" title="Timeline of white dwarfs, neutron stars, and supernovae">Observational timeline</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Particles, forces, <br />and interactions</th><td class="navbox-list-with-group navbox-list navbox-even hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Elementary_particle" title="Elementary particle">Elementary particles</a> <ul><li><a href="/wiki/Proton" title="Proton">Proton</a></li> <li><a href="/wiki/Neutron" title="Neutron">Neutron</a></li> <li><a href="/wiki/Electron" title="Electron">Electron</a></li> <li><a href="/wiki/Neutrino" title="Neutrino">Neutrino</a></li></ul></li> <li><a href="/wiki/Fundamental_interaction" title="Fundamental interaction">Fundamental interactions</a> <ul><li><a href="/wiki/Strong_interaction" title="Strong interaction">Strong interaction</a></li> <li><a href="/wiki/Weak_interaction" title="Weak interaction">Weak interaction</a></li> <li><a href="/wiki/Gravitation" class="mw-redirect" title="Gravitation">Gravitation</a></li></ul></li></ul> <ul><li><a href="/wiki/Pair_production" title="Pair production">Pair production</a></li> <li><a href="/wiki/Inverse_beta_decay" title="Inverse beta decay">Inverse beta decay (electron capture)</a></li> <li><a href="/wiki/Degeneracy_pressure" class="mw-redirect" title="Degeneracy pressure">Degeneracy pressure</a></li> <li><a href="/wiki/Electron_degeneracy_pressure" title="Electron degeneracy pressure">Electron degeneracy pressure</a></li> <li><a href="/wiki/Pauli_exclusion_principle" title="Pauli exclusion principle">Pauli exclusion principle</a></li> <li><b><a href="/wiki/Template:Nuclear_processes" title="Template:Nuclear processes">More...</a></b></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Quantum_mechanics" title="Quantum mechanics">Quantum theory</a></th><td class="navbox-list-with-group navbox-list navbox-odd hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Quantum_mechanics" title="Quantum mechanics">Quantum mechanics</a> <ul><li><a href="/wiki/Introduction_to_quantum_mechanics" title="Introduction to quantum mechanics">Introduction</a></li> <li><a href="/wiki/Basic_concepts_of_quantum_mechanics" class="mw-redirect" title="Basic concepts of quantum mechanics">Basic concepts</a></li></ul></li> <li><a href="/wiki/Quantum_electrodynamics" title="Quantum electrodynamics">Quantum electrodynamics</a></li> <li><a href="/wiki/Quantum_hydrodynamics" title="Quantum hydrodynamics">Quantum hydrodynamics</a></li> <li><a href="/wiki/Quantum_chromodynamics" title="Quantum chromodynamics">Quantum chromodynamics (QCD)</a></li> <li><a href="/wiki/Lattice_QCD" title="Lattice QCD">Lattice QCD</a></li> <li><a href="/wiki/Color_confinement" title="Color confinement">Color confinement</a></li> <li><a href="/wiki/Deconfinement" title="Deconfinement">Deconfinement</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Degenerate_matter" title="Degenerate matter">Degenerate matter</a></th><td class="navbox-list-with-group navbox-list navbox-even hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Neutronium" title="Neutronium">Neutron matter</a></li> <li><a href="/wiki/QCD_matter" title="QCD matter">QCD matter</a></li> <li><a href="/wiki/Quark_matter" class="mw-redirect" title="Quark matter">Quark matter</a></li> <li><a href="/wiki/Quark%E2%80%93gluon_plasma" title="Quark–gluon plasma">Quark–gluon plasma</a></li> <li><a href="/wiki/Preon_matter" class="mw-redirect" title="Preon matter">Preon matter</a></li> <li><a href="/wiki/Strangelet" title="Strangelet">Strangelet</a></li> <li><a href="/wiki/Strange_matter" title="Strange matter">Strange matter</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Related topics</th><td class="navbox-list-with-group navbox-list navbox-odd hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Astronomy" title="Astronomy">Astronomy</a></li> <li><a href="/wiki/Astrophysics" title="Astrophysics">Astrophysics</a></li> <li><a href="/wiki/Nuclear_astrophysics" title="Nuclear astrophysics">Nuclear astrophysics</a></li> <li><a href="/wiki/Physical_cosmology" title="Physical cosmology">Physical cosmology</a></li> <li><a href="/wiki/Shock_wave" title="Shock wave">Physics of shock waves</a></li></ul> </div></td></tr><tr><td class="navbox-abovebelow hlist" colspan="3"><div> <ul><li><span class="nowrap"><span class="noviewer" typeof="mw:File"><a href="/wiki/File:He1523a.jpg" class="mw-file-description"><img alt="icon" src="//upload.wikimedia.org/wikipedia/commons/thumb/5/5f/He1523a.jpg/14px-He1523a.jpg" decoding="async" width="14" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/5/5f/He1523a.jpg/21px-He1523a.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/5/5f/He1523a.jpg/28px-He1523a.jpg 2x" data-file-width="180" data-file-height="207" /></a></span> </span><a href="/wiki/Portal:Stars" title="Portal:Stars">Stars portal</a></li></ul> </div></td></tr></tbody></table></div> <div class="navbox-styles"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1129693374"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236075235"></div><div role="navigation" class="navbox" aria-labelledby="Stars520" style="padding:3px"><table class="nowraplinks hlist mw-collapsible mw-collapsed navbox-inner" style="border-spacing:0;background:transparent;color:inherit"><tbody><tr><th scope="col" class="navbox-title" colspan="2"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1129693374"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1239400231"><div class="navbar plainlinks hlist navbar-mini"><ul><li class="nv-view"><a href="/wiki/Template:Star" title="Template:Star"><abbr title="View this template">v</abbr></a></li><li class="nv-talk"><a href="/wiki/Template_talk:Star" title="Template talk:Star"><abbr title="Discuss this template">t</abbr></a></li><li class="nv-edit"><a href="/wiki/Special:EditPage/Template:Star" title="Special:EditPage/Template:Star"><abbr title="Edit this template">e</abbr></a></li></ul></div><div id="Stars520" style="font-size:114%;margin:0 4em"><a href="/wiki/Star" title="Star">Stars</a></div></th></tr><tr><td class="navbox-abovebelow" colspan="2"><div> <ul><li><a href="/wiki/Lists_of_stars" title="Lists of stars">List</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Star_formation" title="Star formation">Formation</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Accretion_(astrophysics)" title="Accretion (astrophysics)">Accretion</a></li> <li><a href="/wiki/Molecular_cloud" title="Molecular cloud">Molecular cloud</a></li> <li><a href="/wiki/Bok_globule" title="Bok globule">Bok globule</a></li> <li><a href="/wiki/Young_stellar_object" title="Young stellar object">Young stellar object</a> <ul><li><a href="/wiki/Protostar" title="Protostar">Protostar</a></li> <li><a href="/wiki/Pre-main-sequence_star" title="Pre-main-sequence star">Pre-main-sequence</a></li> <li><a href="/wiki/Herbig_Ae/Be_star" title="Herbig Ae/Be star">Herbig Ae/Be</a></li> <li><a href="/wiki/T_Tauri_star" title="T Tauri star">T Tauri</a></li></ul></li> <li><a href="/wiki/Herbig%E2%80%93Haro_object" title="Herbig–Haro object">Herbig–Haro object</a></li> <li><a href="/wiki/Hayashi_track" title="Hayashi track">Hayashi track</a></li> <li><a href="/wiki/Henyey_track" title="Henyey track">Henyey track</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Stellar_evolution" title="Stellar evolution">Evolution</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Main_sequence" title="Main sequence">Main sequence</a></li> <li><a href="/wiki/Red-giant_branch" title="Red-giant branch">Red-giant branch</a></li> <li><a href="/wiki/Horizontal_branch" title="Horizontal branch">Horizontal branch</a> <ul><li><a href="/wiki/Red_clump" title="Red clump">Red clump</a></li></ul></li> <li><a href="/wiki/Asymptotic_giant_branch" title="Asymptotic giant branch">Asymptotic giant branch</a> <ul><li><a href="/wiki/Post-AGB_star" title="Post-AGB star">post-AGB</a></li> <li><a href="/wiki/Super-AGB_star" title="Super-AGB star">super-AGB</a></li></ul></li> <li><a href="/wiki/Blue_loop" title="Blue loop">Blue loop</a></li> <li><a href="/wiki/Planetary_nebula" title="Planetary nebula">Planetary nebula</a> <ul><li><a href="/wiki/Protoplanetary_nebula" title="Protoplanetary nebula">Protoplanetary</a></li></ul></li> <li><a href="/wiki/Wolf%E2%80%93Rayet_nebula" title="Wolf–Rayet nebula">Wolf–Rayet nebula</a></li> <li><a href="/wiki/PG_1159_star" title="PG 1159 star">PG1159</a></li> <li><a href="/wiki/Dredge-up" title="Dredge-up">Dredge-up</a></li> <li><a href="/wiki/OH/IR_star" title="OH/IR star">OH/IR</a></li> <li><a href="/wiki/Instability_strip" title="Instability strip">Instability strip</a></li> <li><a href="/wiki/Luminous_blue_variable" title="Luminous blue variable">Luminous blue variable</a></li> <li><a href="/wiki/Stellar_population" title="Stellar population">Stellar population</a></li> <li><a href="/wiki/Supernova" title="Supernova">Supernova</a> <ul><li><a href="/wiki/Superluminous_supernova" title="Superluminous supernova">Superluminous</a></li> <li><a href="/wiki/Hypernova" title="Hypernova">Hypernova</a></li></ul></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Stellar_classification" title="Stellar classification">Classification</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"></div><table class="nowraplinks navbox-subgroup" style="border-spacing:0"><tbody><tr><td colspan="2" class="navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Early-type_star" class="mw-redirect" title="Early-type star">Early</a></li> <li><a href="/wiki/Late-type_star" class="mw-redirect" title="Late-type star">Late</a></li> <li>Main sequence <ul><li><a href="/wiki/O-type_main-sequence_star" title="O-type main-sequence star">O</a></li> <li><a href="/wiki/B-type_main-sequence_star" title="B-type main-sequence star">B</a></li> <li><a href="/wiki/A-type_main-sequence_star" title="A-type main-sequence star">A</a></li> <li><a href="/wiki/F-type_main-sequence_star" title="F-type main-sequence star">F</a></li> <li><a href="/wiki/G-type_main-sequence_star" title="G-type main-sequence star">G</a></li> <li><a href="/wiki/K-type_main-sequence_star" title="K-type main-sequence star">K</a></li> <li><a href="/wiki/Red_dwarf" title="Red dwarf">M</a></li></ul></li> <li><a href="/wiki/Subdwarf" title="Subdwarf">Subdwarf</a> <ul><li><a href="/wiki/Subdwarf_O_star" title="Subdwarf O star">O</a></li> <li><a href="/wiki/Subdwarf_B_star" title="Subdwarf B star">B</a></li></ul></li> <li><a href="/wiki/Wolf%E2%80%93Rayet_star" title="Wolf–Rayet star">WR</a></li> <li><a href="/wiki/OB_star" title="OB star">OB</a></li> <li><a href="/wiki/Subgiant" title="Subgiant">Subgiant</a></li> <li><a href="/wiki/Giant_star" title="Giant star">Giant</a> <ul><li><a href="/wiki/Blue_giant" title="Blue giant">Blue</a></li> <li><a href="/wiki/Red_giant" title="Red giant">Red</a></li> <li><a href="/wiki/Yellow_giant" class="mw-redirect" title="Yellow giant">Yellow</a></li></ul></li> <li><a href="/wiki/Bright_giant" class="mw-redirect" title="Bright giant">Bright giant</a></li> <li><a href="/wiki/Supergiant" title="Supergiant">Supergiant</a> <ul><li><a href="/wiki/Blue_supergiant" title="Blue supergiant">Blue</a></li> <li><a href="/wiki/Red_supergiant" title="Red supergiant">Red</a></li> <li><a href="/wiki/Yellow_supergiant" title="Yellow supergiant">Yellow</a></li></ul></li> <li><a href="/wiki/Hypergiant" title="Hypergiant">Hypergiant</a> <ul><li><a href="/wiki/Yellow_hypergiant" title="Yellow hypergiant">Yellow</a></li></ul></li> <li><a href="/wiki/Carbon_star" title="Carbon star">Carbon</a> <ul><li><a href="/wiki/S-type_star" title="S-type star">S</a></li> <li><a href="/wiki/CN_star" title="CN star">CN</a></li> <li><a href="/wiki/CH_star" title="CH star">CH</a></li></ul></li> <li><a href="/wiki/White_dwarf" title="White dwarf">White dwarf</a></li> <li><a href="/wiki/Chemically_peculiar_star" title="Chemically peculiar star">Chemically peculiar</a> <ul><li><a href="/wiki/Am_star" title="Am star">Am</a></li> <li><a href="/wiki/Ap_and_Bp_stars" title="Ap and Bp stars">Ap/Bp</a></li> <li><a href="/wiki/CEMP_star" title="CEMP star">CEMP</a></li> <li><a href="/wiki/Mercury-manganese_star" title="Mercury-manganese star">HgMn</a></li> <li><a href="/wiki/Helium-weak_star" title="Helium-weak star">He-weak</a></li> <li><a href="/wiki/Barium_star" title="Barium star">Barium</a></li> <li><a href="/wiki/Lambda_Bo%C3%B6tis_star" title="Lambda Boötis star">Lambda Boötis</a></li> <li><a href="/wiki/Lead_star" title="Lead star">Lead</a></li> <li><a href="/wiki/Technetium_star" title="Technetium star">Technetium</a></li></ul></li> <li><a href="/wiki/Be_star" title="Be star">Be</a> <ul><li><a href="/wiki/Shell_star" title="Shell star">Shell</a></li></ul></li> <li><a href="/wiki/B(e)_star" title="B(e) star">B[e]</a></li> <li><a href="/wiki/Helium_star" title="Helium star">Helium</a> <ul><li><a href="/wiki/Extreme_helium_star" title="Extreme helium star">Extreme</a></li></ul></li> <li><a href="/wiki/Blue_straggler" title="Blue straggler">Blue straggler</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Compact_star" class="mw-redirect" title="Compact star">Remnants</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Compact_star" class="mw-redirect" title="Compact star">Compact star</a></li> <li><a href="/wiki/IRAS_00500%2B6713" title="IRAS 00500+6713">Parker's star</a></li> <li><a href="/wiki/White_dwarf" title="White dwarf">White dwarf</a> <ul><li><a href="/wiki/Helium_planet" title="Helium planet">Helium planet</a></li></ul></li> <li><a class="mw-selflink selflink">Neutron</a> <ul><li><a href="/wiki/Radio-quiet_neutron_star" title="Radio-quiet neutron star">Radio-quiet</a></li> <li><a href="/wiki/Pulsar" title="Pulsar">Pulsar</a> <ul><li><a href="/wiki/Binary_pulsar" title="Binary pulsar">Binary</a></li> <li><a href="/wiki/X-ray_pulsar" title="X-ray pulsar">X-ray</a></li></ul></li> <li><a href="/wiki/Magnetar" title="Magnetar">Magnetar</a></li></ul></li> <li><a href="/wiki/Stellar_black_hole" title="Stellar black hole">Stellar black hole</a></li> <li><a href="/wiki/X-ray_binary" title="X-ray binary">X-ray binary</a> <ul><li><a href="/wiki/X-ray_burster" title="X-ray burster">Burster</a></li></ul></li> <li><a href="/wiki/Soft_gamma_repeater" title="Soft gamma repeater">SGR</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Hypothetical_star" title="Hypothetical star">Hypothetical</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Blue_dwarf_(red-dwarf_stage)" title="Blue dwarf (red-dwarf stage)">Blue dwarf</a></li> <li><a href="/wiki/Black_dwarf" title="Black dwarf">Black dwarf</a></li> <li><a href="/wiki/Exotic_star" title="Exotic star">Exotic</a> <ul><li><a href="/wiki/Boson_star" class="mw-redirect" title="Boson star">Boson</a></li> <li><a href="/wiki/Electroweak_star" class="mw-redirect" title="Electroweak star">Electroweak</a></li> <li><a href="/wiki/Strange_star" title="Strange star">Strange</a></li> <li><a href="/wiki/Preon_star" class="mw-redirect" title="Preon star">Preon</a></li> <li><a href="/wiki/Planck_star" title="Planck star">Planck</a></li> <li><a href="/wiki/Dark_star_(dark_matter)" title="Dark star (dark matter)">Dark</a></li> <li><a href="/wiki/Dark-energy_star" title="Dark-energy star">Dark-energy</a></li> <li><a href="/wiki/Quark_star" title="Quark star">Quark</a></li> <li><a href="/wiki/Q_star" title="Q star">Q</a></li></ul></li> <li>Black hole star <ul><li><a href="/wiki/Black_star_(semiclassical_gravity)" title="Black star (semiclassical gravity)">Black</a></li> <li>Hawking</li> <li><a href="/wiki/Quasi-star" title="Quasi-star">Quasi-star</a></li></ul></li> <li><a href="/wiki/Gravastar" title="Gravastar">Gravastar</a></li> <li><a href="/wiki/Thorne%E2%80%93%C5%BBytkow_object" title="Thorne–Żytkow object">Thorne–Żytkow object</a></li> <li><a href="/wiki/Iron_star" title="Iron star">Iron</a></li> <li><a href="/wiki/Blitzar" title="Blitzar">Blitzar</a></li> <li><a href="/wiki/White_hole" title="White hole">White hole</a></li></ul> </div></td></tr></tbody></table><div></div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Stellar_nucleosynthesis" title="Stellar nucleosynthesis">Nucleosynthesis</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Deuterium_fusion" title="Deuterium fusion">Deuterium burning</a></li> <li><a href="/wiki/Lithium_burning" title="Lithium burning">Lithium burning</a></li> <li><a href="/wiki/Proton%E2%80%93proton_chain" title="Proton–proton chain">Proton–proton chain</a></li> <li><a href="/wiki/CNO_cycle" title="CNO cycle">CNO cycle</a></li> <li><a href="/wiki/Helium_flash" title="Helium flash">Helium flash</a></li> <li><a href="/wiki/Triple-alpha_process" title="Triple-alpha process">Triple-alpha process</a></li> <li><a href="/wiki/Alpha_process" title="Alpha process">Alpha process</a></li> <li><a href="/wiki/Carbon-burning_process" title="Carbon-burning process">C burning</a></li> <li><a href="/wiki/Neon-burning_process" title="Neon-burning process">Ne burning</a></li> <li><a href="/wiki/Oxygen-burning_process" title="Oxygen-burning process">O burning</a></li> <li><a href="/wiki/Silicon-burning_process" title="Silicon-burning process">Si burning</a></li> <li><a href="/wiki/S-process" title="S-process">s-process</a></li> <li><a href="/wiki/R-process" title="R-process">r-process</a></li> <li><a href="/wiki/P-process" title="P-process">p-process</a></li> <li><a href="/wiki/Nova" title="Nova">Nova</a> <ul><li><a href="/wiki/Symbiotic_nova" title="Symbiotic nova">Symbiotic</a></li> <li><a href="/wiki/Nova_remnant" title="Nova remnant">Remnant</a></li> <li><a href="/wiki/Luminous_red_nova" title="Luminous red nova">Luminous red nova</a></li> <li><a href="/wiki/Nova#Recurrent_novae" title="Nova">Recurrent</a></li> <li><a href="/wiki/Micronova" title="Micronova">Micronova</a></li></ul></li> <li><a href="/wiki/Supernova_nucleosynthesis" title="Supernova nucleosynthesis">Supernova</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Stellar_structure" title="Stellar structure">Structure</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Stellar_core" title="Stellar core">Core</a></li> <li><a href="/wiki/Convection_zone" title="Convection zone">Convection zone</a> <ul><li><a href="/wiki/Microturbulence" title="Microturbulence">Microturbulence</a></li> <li><a href="/wiki/Solar-like_oscillations" title="Solar-like oscillations">Oscillations</a></li></ul></li> <li><a href="/wiki/Radiation_zone" class="mw-redirect" title="Radiation zone">Radiation zone</a></li> <li><a href="/wiki/Stellar_atmosphere" title="Stellar atmosphere">Atmosphere</a> <ul><li><a href="/wiki/Photosphere" title="Photosphere">Photosphere</a></li> <li><a href="/wiki/Starspot" title="Starspot">Starspot</a></li> <li><a href="/wiki/Chromosphere" title="Chromosphere">Chromosphere</a></li> <li><a href="/wiki/Stellar_corona" title="Stellar corona">Stellar corona</a></li> <li><a href="/wiki/Alfv%C3%A9n_surface" title="Alfvén surface">Alfvén surface</a></li></ul></li> <li><a href="/wiki/Stellar_wind" title="Stellar wind">Stellar wind</a> <ul><li><a href="/wiki/Stellar-wind_bubble" title="Stellar-wind bubble">Bubble</a></li> <li><a href="/wiki/Bipolar_outflow" title="Bipolar outflow">Bipolar outflow</a></li></ul></li> <li><a href="/wiki/Accretion_disk" title="Accretion disk">Accretion disk</a> <ul><li><a href="/wiki/Protoplanetary_disk" title="Protoplanetary disk">Protoplanetary disk</a></li> <li><a href="/wiki/Proplyd" title="Proplyd">Proplyd</a></li></ul></li> <li><a href="/wiki/Asteroseismology" title="Asteroseismology">Asteroseismology</a> <ul><li><a href="/wiki/Helioseismology" title="Helioseismology">Helioseismology</a></li></ul></li> <li><a href="/wiki/Circumstellar_dust" title="Circumstellar dust">Circumstellar dust</a></li> <li><a href="/wiki/Cosmic_dust" title="Cosmic dust">Cosmic dust</a></li> <li><a href="/wiki/Circumstellar_envelope" title="Circumstellar envelope">Circumstellar envelope</a></li> <li><a href="/wiki/Eddington_luminosity" title="Eddington luminosity">Eddington luminosity</a></li> <li><a href="/wiki/Kelvin%E2%80%93Helmholtz_mechanism" title="Kelvin–Helmholtz mechanism">Kelvin–Helmholtz mechanism</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Properties</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Stellar_designations_and_names" title="Stellar designations and names">Designation</a></li> <li><a href="/wiki/Stellar_dynamics" title="Stellar dynamics">Dynamics</a></li> <li><a href="/wiki/Effective_temperature" title="Effective temperature">Effective temperature</a></li> <li><a href="/wiki/Luminosity" title="Luminosity">Luminosity</a></li> <li><a href="/wiki/Stellar_kinematics" title="Stellar kinematics">Kinematics</a></li> <li><a href="/wiki/Stellar_magnetic_field" title="Stellar magnetic field">Magnetic field</a></li> <li><a href="/wiki/Absolute_magnitude" title="Absolute magnitude">Absolute magnitude</a></li> <li><a href="/wiki/Stellar_mass" title="Stellar mass">Mass</a></li> <li><a href="/wiki/Metallicity" title="Metallicity">Metallicity</a></li> <li><a href="/wiki/Stellar_rotation" title="Stellar rotation">Rotation</a></li> <li><a href="/wiki/Starlight" title="Starlight">Starlight</a></li> <li><a href="/wiki/Variable_star" title="Variable star">Variable</a></li> <li><a href="/wiki/Photometric_system" title="Photometric system">Photometric system</a></li> <li><a href="/wiki/Color_index" title="Color index">Color index</a></li> <li><a href="/wiki/Hertzsprung%E2%80%93Russell_diagram" title="Hertzsprung–Russell diagram">Hertzsprung–Russell diagram</a></li> <li><a href="/wiki/Color%E2%80%93color_diagram" title="Color–color diagram">Color–color diagram</a></li> <li><a href="/wiki/Str%C3%B6mgren_sphere" title="Strömgren sphere">Strömgren sphere</a></li> <li><a href="/wiki/Kraft_break" title="Kraft break">Kraft break</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Star_system" title="Star system">Star systems</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Binary_star" title="Binary star">Binary</a> <ul><li><a href="/wiki/Contact_binary" title="Contact binary">Contact</a></li> <li><a href="/wiki/Common_envelope" title="Common envelope">Common envelope</a></li> <li><a href="/wiki/Eclipsing_binary" class="mw-redirect" title="Eclipsing binary">Eclipsing</a></li> <li><a href="/wiki/Symbiotic_binary" title="Symbiotic binary">Symbiotic</a></li></ul></li> <li><a href="/wiki/Star_system#Multiple_star_systems" title="Star system">Multiple</a></li> <li><a href="/wiki/Star_cluster" title="Star cluster">Cluster</a> <ul><li><a href="/wiki/Open_cluster" title="Open cluster">Open</a></li> <li><a href="/wiki/Globular_cluster" title="Globular cluster">Globular</a></li> <li><a href="/wiki/Super_star_cluster" title="Super star cluster">Super</a></li></ul></li> <li><a href="/wiki/Planetary_system" title="Planetary system">Planetary system</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Earth-centric<br />observations</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Sun" title="Sun">Sun</a> <ul><li><a href="/wiki/Solar_eclipse" title="Solar eclipse">Solar eclipse</a></li> <li><a href="/wiki/Solar_radio_emission" title="Solar radio emission">Solar radio emission</a></li> <li><a href="/wiki/Solar_System" title="Solar System">Solar System</a></li> <li><a href="/wiki/Sunlight" title="Sunlight">Sunlight</a></li></ul></li> <li><a href="/wiki/Pole_star" title="Pole star">Pole star</a></li> <li><a href="/wiki/Circumpolar_star" title="Circumpolar star">Circumpolar</a></li> <li><a href="/wiki/Constellation" title="Constellation">Constellation</a></li> <li><a href="/wiki/Asterism_(astronomy)" title="Asterism (astronomy)">Asterism</a></li> <li><a href="/wiki/Magnitude_(astronomy)" title="Magnitude (astronomy)">Magnitude</a> <ul><li><a href="/wiki/Apparent_magnitude" title="Apparent magnitude">Apparent</a></li> <li><a href="/wiki/Extinction_(astronomy)" title="Extinction (astronomy)">Extinction</a></li> <li><a href="/wiki/Photographic_magnitude" title="Photographic magnitude">Photographic</a></li></ul></li> <li><a href="/wiki/Radial_velocity" title="Radial velocity">Radial velocity</a></li> <li><a href="/wiki/Proper_motion" title="Proper motion">Proper motion</a></li> <li><a href="/wiki/Stellar_parallax" title="Stellar parallax">Parallax</a></li> <li><a href="/wiki/Photometric-standard_star" title="Photometric-standard star">Photometric-standard</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Lists_of_stars" title="Lists of stars">Lists</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/List_of_proper_names_of_stars" title="List of proper names of stars">Proper names</a> <ul><li><a href="/wiki/List_of_Arabic_star_names" title="List of Arabic star names">Arabic</a></li> <li><a href="/wiki/Chinese_star_names" class="mw-redirect" title="Chinese star names">Chinese</a></li></ul></li> <li><a href="/wiki/List_of_star_extremes" title="List of star extremes">Extremes</a> <ul><li><a href="/wiki/List_of_most_massive_stars" title="List of most massive stars">Most massive</a></li> <li><a href="/wiki/List_of_hottest_stars" title="List of hottest stars">Highest temperature</a></li> <li><a href="/wiki/List_of_coolest_stars" title="List of coolest stars">Lowest temperature</a></li> <li><a href="/wiki/List_of_largest_known_stars" class="mw-redirect" title="List of largest known stars">Largest volume</a></li> <li><a href="/wiki/List_of_smallest_known_stars" title="List of smallest known stars">Smallest volume</a></li> <li><a href="/wiki/List_of_brightest_stars" title="List of brightest stars">Brightest</a></li> <li><a href="/wiki/Historical_brightest_stars" title="Historical brightest stars">Historical brightest</a></li> <li><a href="/wiki/List_of_most_luminous_stars" title="List of most luminous stars">Most luminous</a></li> <li><a href="/wiki/List_of_nearest_stars" title="List of nearest stars">Nearest</a> <ul><li><a href="/wiki/List_of_nearest_bright_stars" title="List of nearest bright stars">bright</a></li></ul></li> <li><a href="/wiki/List_of_the_most_distant_astronomical_objects#List_of_most_distant_objects_by_type" title="List of the most distant astronomical objects">Most distant</a></li></ul></li> <li><a href="/wiki/List_of_stars_with_resolved_images" title="List of stars with resolved images">With resolved images</a></li> <li><a href="/wiki/List_of_multiplanetary_systems" title="List of multiplanetary systems">With multiple exoplanets</a></li> <li><a href="/wiki/List_of_brown_dwarfs" title="List of brown dwarfs">Brown dwarfs</a></li> <li><a href="/wiki/List_of_red_dwarfs" title="List of red dwarfs">Red dwarfs</a></li> <li><a href="/wiki/List_of_white_dwarfs" title="List of white dwarfs">White dwarfs</a></li> <li><a href="/wiki/List_of_novae_in_the_Milky_Way_galaxy" title="List of novae in the Milky Way galaxy">Milky Way novae</a></li> <li><a href="/wiki/List_of_supernovae" title="List of supernovae">Supernovae</a> <ul><li><a href="/wiki/List_of_supernova_candidates" title="List of supernova candidates">Candidates</a></li> <li><a href="/wiki/List_of_supernova_remnants" title="List of supernova remnants">Remnants</a></li></ul></li> <li><a href="/wiki/List_of_planetary_nebulae" title="List of planetary nebulae">Planetary nebulae</a></li> <li><a href="/wiki/Timeline_of_stellar_astronomy" title="Timeline of stellar astronomy">Timeline of stellar astronomy</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Related</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Substellar_object" title="Substellar object">Substellar object</a> <ul><li><a href="/wiki/Brown_dwarf" title="Brown dwarf">Brown dwarf</a> <ul><li><a href="/wiki/Brown-dwarf_desert" title="Brown-dwarf desert">Desert</a></li> <li><a href="/wiki/Sub-brown_dwarf" title="Sub-brown dwarf">Sub</a></li></ul></li> <li><a href="/wiki/Planet" title="Planet">Planet</a></li></ul></li> <li><a href="/wiki/Galactic_year" title="Galactic year">Galactic year</a></li> <li><a href="/wiki/Galaxy" title="Galaxy">Galaxy</a></li> <li><a href="/wiki/Guest_star_(astronomy)" title="Guest star (astronomy)">Guest</a></li> <li><a href="/wiki/Gravity" title="Gravity">Gravity</a></li> <li><a href="/wiki/Intergalactic_star" title="Intergalactic star">Intergalactic</a></li> <li><a href="/wiki/Planet-hosting_stars" class="mw-redirect" title="Planet-hosting stars">Planet-hosting stars</a></li> <li><a href="/wiki/Tidal_disruption_event" title="Tidal disruption event">Tidal disruption event</a></li></ul> </div></td></tr><tr><td class="navbox-abovebelow" colspan="2"><div> <ul><li><span class="noviewer" typeof="mw:File"><span title="Category"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/16px-Symbol_category_class.svg.png" decoding="async" width="16" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/23px-Symbol_category_class.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/31px-Symbol_category_class.svg.png 2x" data-file-width="180" data-file-height="185" /></span></span> <a href="/wiki/Category:Stars" title="Category:Stars">Category</a></li> <li><span class="nowrap"><span class="noviewer" typeof="mw:File"><a href="/wiki/File:He1523a.jpg" class="mw-file-description"><img alt="icon" src="//upload.wikimedia.org/wikipedia/commons/thumb/5/5f/He1523a.jpg/14px-He1523a.jpg" decoding="async" width="14" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/5/5f/He1523a.jpg/21px-He1523a.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/5/5f/He1523a.jpg/28px-He1523a.jpg 2x" data-file-width="180" data-file-height="207" /></a></span> </span><a href="/wiki/Portal:Stars" title="Portal:Stars">Stars portal</a></li></ul> </div></td></tr></tbody></table></div> <div class="navbox-styles"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1129693374"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236075235"></div><div role="navigation" class="navbox" aria-labelledby="Supernovae316" style="padding:3px"><table class="nowraplinks hlist mw-collapsible autocollapse navbox-inner" style="border-spacing:0;background:transparent;color:inherit"><tbody><tr><th scope="col" class="navbox-title" colspan="3"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1129693374"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1239400231"><div class="navbar plainlinks hlist navbar-mini"><ul><li class="nv-view"><a href="/wiki/Template:Supernovae" title="Template:Supernovae"><abbr title="View this template">v</abbr></a></li><li class="nv-talk"><a href="/wiki/Template_talk:Supernovae" title="Template talk:Supernovae"><abbr title="Discuss this template">t</abbr></a></li><li class="nv-edit"><a href="/wiki/Special:EditPage/Template:Supernovae" title="Special:EditPage/Template:Supernovae"><abbr title="Edit this template">e</abbr></a></li></ul></div><div id="Supernovae316" style="font-size:114%;margin:0 4em"><a href="/wiki/Supernova" title="Supernova">Supernovae</a></div></th></tr><tr><th scope="row" class="navbox-group" style="width:1%">Classes</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Type_Ia_supernova" title="Type Ia supernova">Type Ia</a></li> <li><a href="/wiki/Type_Iax_supernova" title="Type Iax supernova">Type Iax</a></li> <li><a href="/wiki/Type_Ib_and_Ic_supernovae" title="Type Ib and Ic supernovae">Type Ib and Ic</a></li> <li><a href="/wiki/Type_II_supernova" title="Type II supernova">Type II (IIP, IIL, IIn, and IIb)</a></li> <li><a href="/wiki/Hypernova" title="Hypernova">Hypernova</a></li> <li><a href="/wiki/Superluminous_supernova" title="Superluminous supernova">Superluminous</a></li> <li><a href="/wiki/Pair-instability_supernova" title="Pair-instability supernova">Pair-instability</a></li> <li><a href="/wiki/Calcium-rich_supernovae" class="mw-redirect" title="Calcium-rich supernovae">Calcium-rich</a></li> <li><a href="/wiki/Common_envelope_jets_supernova" title="Common envelope jets supernova">Common envelope jets supernova</a></li></ul> </div></td><td class="noviewer navbox-image" rowspan="9" style="width:1px;padding:0 0 0 2px"><div><span typeof="mw:File"><a href="/wiki/File:G299-Remnants-SuperNova-Type1a-20150218.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/b/bd/G299-Remnants-SuperNova-Type1a-20150218.jpg/180px-G299-Remnants-SuperNova-Type1a-20150218.jpg" decoding="async" width="180" height="180" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/b/bd/G299-Remnants-SuperNova-Type1a-20150218.jpg/270px-G299-Remnants-SuperNova-Type1a-20150218.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/b/bd/G299-Remnants-SuperNova-Type1a-20150218.jpg/360px-G299-Remnants-SuperNova-Type1a-20150218.jpg 2x" data-file-width="946" data-file-height="946" /></a></span></div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Physics of</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Carbon_detonation" title="Carbon detonation">Carbon detonation</a></li> <li><a href="/wiki/Foe_(unit)" title="Foe (unit)">Foe/Bethe</a></li> <li><a href="/wiki/Near-Earth_supernova" title="Near-Earth supernova">Near-Earth</a></li> <li><a href="/wiki/Phillips_relationship" title="Phillips relationship">Phillips relationship</a></li> <li><a href="/wiki/Supernova_nucleosynthesis" title="Supernova nucleosynthesis">Nucleosynthesis</a> <ul><li><a href="/wiki/P-process" title="P-process">p-process</a></li> <li><a href="/wiki/R-process" title="R-process">r-process</a></li> <li><a href="/wiki/Gamma_process_(astrophysics)" class="mw-redirect" title="Gamma process (astrophysics)">γ-process</a></li></ul></li> <li><a href="/wiki/Supernova_neutrinos" title="Supernova neutrinos">Neutrinos</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Related</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Failed_supernova" title="Failed supernova">Failed</a></li> <li><a href="/wiki/Fast_blue_optical_transient" title="Fast blue optical transient">Fast blue optical transient</a></li> <li><a href="/wiki/Fast_radio_burst" title="Fast radio burst">Fast radio burst</a></li> <li><a href="/wiki/Gamma-ray_burst" title="Gamma-ray burst">Gamma-ray burst</a></li> <li><a href="/wiki/Gravitational_wave" title="Gravitational wave">Gravitational wave</a></li> <li><a href="/wiki/Kilonova" title="Kilonova">Kilonova</a></li> <li><a href="/wiki/Luminous_red_nova" title="Luminous red nova">Luminous red nova</a></li> <li><a href="/wiki/Micronova" title="Micronova">Micronova</a></li> <li><a href="/wiki/Nova" title="Nova">Nova</a></li> <li><a href="/wiki/Pulsar_kick" title="Pulsar kick">Pulsar kick</a></li> <li><a href="/wiki/Quark-nova" title="Quark-nova">Quark-nova</a></li> <li><a href="/wiki/Soft_gamma_repeater" title="Soft gamma repeater">Soft gamma repeater</a></li> <li><a href="/wiki/Supernova_impostor" title="Supernova impostor">Imposter</a> <ul><li><a href="/wiki/Pulsational_pair-instability_supernova" title="Pulsational pair-instability supernova">pulsational pair-instability</a></li></ul></li> <li><a href="/wiki/Symbiotic_nova" title="Symbiotic nova">Symbiotic nova</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Progenitors</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Hypergiant" title="Hypergiant">Hypergiant</a> <ul><li><a href="/wiki/Yellow_hypergiant" title="Yellow hypergiant">yellow</a></li> <li><a href="/wiki/Red_hypergiant" class="mw-redirect" title="Red hypergiant">Red</a></li></ul></li> <li><a href="/wiki/Luminous_blue_variable" title="Luminous blue variable">Luminous blue variable</a></li> <li><a href="/wiki/Supergiant_star" class="mw-redirect" title="Supergiant star">Supergiant</a> <ul><li><a href="/wiki/Blue_supergiant_star" class="mw-redirect" title="Blue supergiant star">blue</a></li> <li><a href="/wiki/Red_supergiant_star" class="mw-redirect" title="Red supergiant star">red</a></li> <li><a href="/wiki/Yellow_supergiant_star" class="mw-redirect" title="Yellow supergiant star">yellow</a></li></ul></li> <li><a href="/wiki/White_dwarf" title="White dwarf">White dwarf</a></li> <li><a href="/wiki/Wolf%E2%80%93Rayet_star" title="Wolf–Rayet star">Wolf–Rayet star</a></li> <li><a href="/wiki/Super-AGB_star" title="Super-AGB star">Super-AGB star</a></li> <li><a href="/wiki/Population_III_star" class="mw-redirect" title="Population III star">Population III star</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Remnants</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Supernova_remnant" title="Supernova remnant">Supernova remnant</a> <ul><li><a href="/wiki/Pulsar_wind_nebula" title="Pulsar wind nebula">Pulsar wind nebula</a></li></ul></li> <li><a class="mw-selflink selflink">Neutron star</a> <ul><li><a href="/wiki/Pulsar" title="Pulsar">pulsar</a></li> <li><a href="/wiki/Magnetar" title="Magnetar">magnetar</a></li></ul></li> <li><a href="/wiki/Stellar_black_hole" title="Stellar black hole">Stellar black hole</a></li> <li><a href="/wiki/Compact_star" class="mw-redirect" title="Compact star">Compact star</a> <ul><li><a href="/wiki/Electroweak_star" class="mw-redirect" title="Electroweak star">electroweak</a></li> <li><a href="/wiki/Exotic_star" title="Exotic star">exotic</a></li> <li><a href="/wiki/Quark_star" title="Quark star">quark</a></li></ul></li> <li><a href="/wiki/Zombie_star" class="mw-redirect" title="Zombie star">Zombie star</a></li> <li><a href="/wiki/Local_Bubble" title="Local Bubble">Local Bubble</a></li> <li><a href="/wiki/Superbubble" title="Superbubble">Superbubble</a> <ul><li><a href="/wiki/Orion%E2%80%93Eridanus_Superbubble" title="Orion–Eridanus Superbubble">Orion–Eridanus</a></li></ul></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Discovery</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Guest_star_(astronomy)" title="Guest star (astronomy)">Guest star</a></li> <li><a href="/wiki/History_of_supernova_observation" title="History of supernova observation">History of supernova observation</a></li> <li><a href="/wiki/Timeline_of_white_dwarfs,_neutron_stars,_and_supernovae" title="Timeline of white dwarfs, neutron stars, and supernovae">Timeline of white dwarfs, neutron stars, and supernovae</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Lists</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/List_of_supernova_candidates" title="List of supernova candidates">Candidates</a></li> <li><a href="/wiki/List_of_supernovae" title="List of supernovae">Notable</a></li> <li><a href="/wiki/List_of_most_massive_stars" title="List of most massive stars">Massive stars</a></li> <li><a href="/wiki/List_of_most_distant_supernovae" title="List of most distant supernovae">Most distant</a></li> <li><a href="/wiki/List_of_supernova_remnants" title="List of supernova remnants">Remnants</a></li> <li><a href="/wiki/Supernovae_in_fiction" title="Supernovae in fiction">In fiction</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Notable</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Barnard%27s_Loop" title="Barnard's Loop">Barnard's Loop</a></li> <li><a href="/wiki/Cassiopeia_A" title="Cassiopeia A">Cassiopeia A</a></li> <li><a href="/wiki/SN_1054" title="SN 1054">SN 1054</a> <ul><li><a href="/wiki/Crab_Nebula" title="Crab Nebula">Crab Nebula</a></li></ul></li> <li><a href="/wiki/IPTF14hls" title="IPTF14hls">iPTF14hls</a></li> <li><a href="/wiki/SN_1000%2B0216" title="SN 1000+0216">SN 1000+0216</a></li> <li><a href="/wiki/SN_1572" title="SN 1572">Tycho's</a></li> <li><a href="/wiki/Kepler%27s_Supernova" title="Kepler's Supernova">Kepler's</a></li> <li><a href="/wiki/SN_1885A" title="SN 1885A">SN 1885A</a></li> <li><a href="/wiki/SN_1987A" title="SN 1987A">SN 1987A</a></li> <li><a href="/wiki/SN_1994D" title="SN 1994D">SN 1994D</a></li> <li><a href="/wiki/SN_185" title="SN 185">SN 185</a></li> <li><a href="/wiki/SN_1006" title="SN 1006">SN 1006</a></li> <li><a href="/wiki/SN_2003fg" title="SN 2003fg">SN 2003fg</a></li> <li><a href="/wiki/G1.9%2B0.3" title="G1.9+0.3">Remnant G1.9+0.3</a></li> <li><a href="/wiki/SN_2007bi" title="SN 2007bi">SN 2007bi</a></li> <li><a href="/wiki/SN_2011fe" title="SN 2011fe">SN 2011fe</a></li> <li><a href="/wiki/SN_2014J" title="SN 2014J">SN 2014J</a></li> <li><a href="/wiki/SN_Refsdal" title="SN Refsdal">SN Refsdal</a></li> <li><a href="/wiki/Vela_Supernova_Remnant" title="Vela Supernova Remnant">Vela Remnant</a></li> <li><a href="/wiki/SN_2006gy" title="SN 2006gy">SN 2006gy</a></li> <li><a href="/wiki/ASASSN-15lh" title="ASASSN-15lh">ASASSN-15lh</a></li> <li><a href="/wiki/SN_2016aps" title="SN 2016aps">SN 2016aps</a></li> <li><a href="/wiki/SN_2018cow" title="SN 2018cow">SN 2018cow</a></li> <li><a href="/wiki/SN_2022jli" title="SN 2022jli">SN 2022jli</a></li> <li><a href="/wiki/SN_H0pe" title="SN H0pe">SN H0pe</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Research</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/All_Sky_Automated_Survey_for_SuperNovae" title="All Sky Automated Survey for SuperNovae">ASAS-SN</a></li> <li><a href="/wiki/Cal%C3%A1n/Tololo_Survey" title="Calán/Tololo Survey">Calán/Tololo Survey</a></li> <li><a href="/wiki/High-Z_Supernova_Search_Team" title="High-Z Supernova Search Team">High-Z Supernova Search Team</a></li> <li><a href="/wiki/Katzman_Automatic_Imaging_Telescope" title="Katzman Automatic Imaging Telescope">Katzman Automatic Imaging Telescope</a></li> <li><a href="/wiki/Monte_Agliale_Supernovae_and_Asteroid_Survey" title="Monte Agliale Supernovae and Asteroid Survey">Monte Agliale Supernovae and Asteroid Survey</a></li> <li><a href="/wiki/Nearby_Supernova_Factory" title="Nearby Supernova Factory">Nearby Supernova Factory</a></li> <li><a href="/wiki/Sloan_Digital_Sky_Survey#Sloan_Supernova_Survey" title="Sloan Digital Sky Survey">Sloan Supernova Survey</a></li> <li><a href="/wiki/Supernova/Acceleration_Probe" class="mw-redirect" title="Supernova/Acceleration Probe">Supernova/Acceleration Probe</a></li> <li><a href="/wiki/Supernova_Cosmology_Project" title="Supernova Cosmology Project">Supernova Cosmology Project</a></li> <li><a href="/wiki/SuperNova_Early_Warning_System" title="SuperNova Early Warning System">SuperNova Early Warning System</a></li> <li><a href="/wiki/Supernova_Legacy_Survey" title="Supernova Legacy Survey">Supernova Legacy Survey</a></li> <li><a href="/wiki/Texas_Supernova_Search" title="Texas Supernova Search">Texas Supernova Search</a></li></ul> </div></td></tr><tr><td class="navbox-abovebelow" colspan="3"><div> <ul><li><span class="noviewer" typeof="mw:File"><span title="Category"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/16px-Symbol_category_class.svg.png" decoding="async" width="16" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/23px-Symbol_category_class.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/31px-Symbol_category_class.svg.png 2x" data-file-width="180" data-file-height="185" /></span></span> <a href="/wiki/Category:Supernovae" title="Category:Supernovae">Category:Supernovae</a></li> <li><span class="noviewer" typeof="mw:File"><span title="Commons page"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/4/4a/Commons-logo.svg/12px-Commons-logo.svg.png" decoding="async" width="12" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/4/4a/Commons-logo.svg/18px-Commons-logo.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/4/4a/Commons-logo.svg/24px-Commons-logo.svg.png 2x" data-file-width="1024" data-file-height="1376" /></span></span> <a href="https://commons.wikimedia.org/wiki/Category:Supernovae" class="extiw" title="commons:Category:Supernovae">Commons:Supernovae</a></li></ul> </div></td></tr></tbody></table></div> <div class="navbox-styles"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1129693374"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236075235"></div><div role="navigation" class="navbox" aria-labelledby="Gravitational-wave_astronomy227" style="padding:3px"><table class="nowraplinks hlist mw-collapsible mw-collapsed navbox-inner" style="border-spacing:0;background:transparent;color:inherit"><tbody><tr><th scope="col" class="navbox-title" colspan="2"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1129693374"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1239400231"><div class="navbar plainlinks hlist navbar-mini"><ul><li class="nv-view"><a href="/wiki/Template:Gravitational_waves" title="Template:Gravitational waves"><abbr title="View this template">v</abbr></a></li><li class="nv-talk"><a href="/wiki/Template_talk:Gravitational_waves" title="Template talk:Gravitational waves"><abbr title="Discuss this template">t</abbr></a></li><li class="nv-edit"><a href="/wiki/Special:EditPage/Template:Gravitational_waves" title="Special:EditPage/Template:Gravitational waves"><abbr title="Edit this template">e</abbr></a></li></ul></div><div id="Gravitational-wave_astronomy227" style="font-size:114%;margin:0 4em"><a href="/wiki/Gravitational-wave_astronomy" title="Gravitational-wave astronomy">Gravitational-wave astronomy</a></div></th></tr><tr><td class="navbox-abovebelow" colspan="2"><div> <ul><li><a href="/wiki/Gravitational_wave" title="Gravitational wave">Gravitational wave</a></li> <li><a href="/wiki/Gravitational-wave_observatory" title="Gravitational-wave observatory">Gravitational-wave observatory</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Gravitational-wave_observatory" title="Gravitational-wave observatory">Detectors</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"></div><table class="nowraplinks navbox-subgroup" style="border-spacing:0"><tbody><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Gravitational-wave_observatory#Weber_bars" title="Gravitational-wave observatory">Resonant mass<br /> antennas</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"></div><table class="nowraplinks navbox-subgroup" style="border-spacing:0"><tbody><tr><th scope="row" class="navbox-group" style="width:1%">Active</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/w/index.php?title=NAUTILUS&action=edit&redlink=1" class="new" title="NAUTILUS (page does not exist)">NAUTILUS</a> (<a href="/w/index.php?title=International_Gravitational_Event_Collaboration&action=edit&redlink=1" class="new" title="International Gravitational Event Collaboration (page does not exist)">IGEC</a>)</li> <li><a href="/wiki/AURIGA" title="AURIGA">AURIGA</a> (<a href="/w/index.php?title=International_Gravitational_Event_Collaboration&action=edit&redlink=1" class="new" title="International Gravitational Event Collaboration (page does not exist)">IGEC</a>)</li> <li><a href="/wiki/MiniGrail" title="MiniGrail">MiniGRAIL</a></li> <li><a href="/wiki/Mario_Schenberg_(Gravitational_Wave_Detector)" title="Mario Schenberg (Gravitational Wave Detector)">Mario Schenberg</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Past</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/w/index.php?title=EXPLORER&action=edit&redlink=1" class="new" title="EXPLORER (page does not exist)">EXPLORER</a> (<a href="/w/index.php?title=International_Gravitational_Event_Collaboration&action=edit&redlink=1" class="new" title="International Gravitational Event Collaboration (page does not exist)">IGEC</a>)</li> <li><a href="/wiki/Allegro_gravitational-wave_detector" title="Allegro gravitational-wave detector">ALLEGRO</a> (<a href="/w/index.php?title=International_Gravitational_Event_Collaboration&action=edit&redlink=1" class="new" title="International Gravitational Event Collaboration (page does not exist)">IGEC</a>)</li> <li><a href="/wiki/NIOBE" title="NIOBE">NIOBE</a> (<a href="/w/index.php?title=International_Gravitational_Event_Collaboration&action=edit&redlink=1" class="new" title="International Gravitational Event Collaboration (page does not exist)">IGEC</a>)</li> <li><a href="/w/index.php?title=Stanford_gravitational_wave_detector&action=edit&redlink=1" class="new" title="Stanford gravitational wave detector (page does not exist)">Stanford gravitational wave detector</a></li> <li><a href="/w/index.php?title=ALTAIR_(gravitational_wave_detector)&action=edit&redlink=1" class="new" title="ALTAIR (gravitational wave detector) (page does not exist)">ALTAIR</a></li> <li><a href="/w/index.php?title=GEOGRAV&action=edit&redlink=1" class="new" title="GEOGRAV (page does not exist)">GEOGRAV</a></li> <li><a href="/w/index.php?title=AGATA_(gravitational_wave_detector)&action=edit&redlink=1" class="new" title="AGATA (gravitational wave detector) (page does not exist)">AGATA</a></li> <li><a href="/wiki/Weber_bar" title="Weber bar">Weber bar</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Proposed</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Torsion-bar_antenna" title="Torsion-bar antenna">TOBA</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Past proposals</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/MiniGrail" title="MiniGrail">GRAIL</a> (downsized to <a href="/wiki/MiniGrail" title="MiniGrail">MiniGRAIL</a>)</li> <li><a href="/w/index.php?title=Truncated_Icosahedral_Gravitational_Wave_Antenna&action=edit&redlink=1" class="new" title="Truncated Icosahedral Gravitational Wave Antenna (page does not exist)">TIGA</a></li> <li><a href="/w/index.php?title=SFERA&action=edit&redlink=1" class="new" title="SFERA (page does not exist)">SFERA</a></li> <li><a href="/wiki/Mario_Schenberg_(Gravitational_Wave_Detector)" title="Mario Schenberg (Gravitational Wave Detector)">Graviton</a> (downsized to <a href="/wiki/Mario_Schenberg_(Gravitational_Wave_Detector)" title="Mario Schenberg (Gravitational Wave Detector)">Mario Schenberg</a>)</li></ul> </div></td></tr></tbody></table><div></div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Ground-based_interferometric_gravitational-wave_search" title="Ground-based interferometric gravitational-wave search"> Ground-based<br />interferometers</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"></div><table class="nowraplinks navbox-subgroup" style="border-spacing:0"><tbody><tr><th scope="row" class="navbox-group" style="width:1%">Active</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/AIGO" title="AIGO">AIGO</a> (<a href="/wiki/ACIGA" title="ACIGA">ACIGA</a>)</li> <li><a href="/wiki/CLIO" title="CLIO">CLIO</a></li> <li><a href="/wiki/Holometer" title="Holometer">Fermilab holometer</a></li> <li><a href="/wiki/GEO600" title="GEO600">GEO600</a></li> <li><a href="/wiki/LIGO" title="LIGO">Advanced LIGO</a> (<a href="/wiki/LIGO_Scientific_Collaboration" title="LIGO Scientific Collaboration">LIGO Scientific Collaboration</a>)</li> <li><a href="/wiki/KAGRA" title="KAGRA">KAGRA</a></li> <li><a href="/wiki/Virgo_interferometer" title="Virgo interferometer">Advanced Virgo</a> (<a href="/wiki/European_Gravitational_Observatory" title="European Gravitational Observatory">European Gravitational Observatory</a>)</li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Past</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/TAMA_300" title="TAMA 300">TAMA 300</a></li> <li><a href="/wiki/TAMA_300" title="TAMA 300">TAMA 20, later known as LISM</a></li> <li><a href="/w/index.php?title=TENKO-100&action=edit&redlink=1" class="new" title="TENKO-100 (page does not exist)">TENKO-100</a></li> <li><a href="/wiki/LIGO#Background" title="LIGO">Caltech 40m interferometer</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Planned</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Indian_Initiative_in_Gravitational-wave_Observations" title="Indian Initiative in Gravitational-wave Observations">INDIGO (LIGO-India)</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Proposed</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Cosmic_Explorer_(gravitational_wave_observatory)" title="Cosmic Explorer (gravitational wave observatory)">Cosmic Explorer</a></li> <li><a href="/wiki/Einstein_Telescope" title="Einstein Telescope">Einstein Telescope</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Past proposals</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/LIGO-Australia" class="mw-redirect" title="LIGO-Australia">LIGO-Australia</a></li></ul> </div></td></tr></tbody></table><div></div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Space-based<br />interferometers</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"></div><table class="nowraplinks navbox-subgroup" style="border-spacing:0"><tbody><tr><th scope="row" class="navbox-group" style="width:1%">Planned</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Laser_Interferometer_Space_Antenna" title="Laser Interferometer Space Antenna">LISA</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Proposed</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Big_Bang_Observer" title="Big Bang Observer">Big Bang Observer</a></li> <li><a href="/wiki/Deci-hertz_Interferometer_Gravitational_wave_Observatory" title="Deci-hertz Interferometer Gravitational wave Observatory">DECIGO</a></li> <li><a href="/wiki/TianQin" title="TianQin">TianQin</a></li></ul> </div></td></tr></tbody></table><div></div></td></tr></tbody></table><div></div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Pulsar_timing_array" title="Pulsar timing array">Pulsar timing arrays</a></th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/European_Pulsar_Timing_Array" title="European Pulsar Timing Array">EPTA</a></li> <li><a href="/wiki/International_Pulsar_Timing_Array" title="International Pulsar Timing Array">IPTA</a></li> <li><a href="/wiki/North_American_Nanohertz_Observatory_for_Gravitational_Waves" title="North American Nanohertz Observatory for Gravitational Waves">NANOGrav</a></li> <li><a href="/wiki/Parkes_Observatory" title="Parkes Observatory">PPTA</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Data analysis</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Einstein@Home" title="Einstein@Home">Einstein@Home</a></li> <li><a href="/wiki/PyCBC" title="PyCBC">PyCBC</a></li> <li><a href="/wiki/Zooniverse" title="Zooniverse">Zooniverse</a>: Gravity Spy</li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Observations</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"></div><table class="nowraplinks navbox-subgroup" style="border-spacing:0"><tbody><tr><th scope="row" class="navbox-group" style="width:1%">Events</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/List_of_gravitational_wave_observations" title="List of gravitational wave observations">List of observations</a></li> <li><a href="/wiki/First_observation_of_gravitational_waves" title="First observation of gravitational waves">First observation (GW150914)</a></li> <li><a href="/wiki/GW151226" title="GW151226">GW151226</a></li> <li><a href="/wiki/GW170104" title="GW170104">GW170104</a></li> <li><a href="/wiki/GW170608" title="GW170608">GW170608</a></li> <li><a href="/wiki/GW170814" title="GW170814">GW170814</a></li> <li><a href="/wiki/GW170817" title="GW170817">GW170817</a> (first <a href="/wiki/Neutron_star_merger" title="Neutron star merger">neutron star merger</a>)</li> <li><a href="/wiki/GW190412" title="GW190412">GW190412</a></li> <li><a href="/wiki/GW190521" title="GW190521">GW190521</a> (first-ever possible light from bh-bh merger)</li> <li><a href="/wiki/GW190814" title="GW190814">GW190814</a> (first-ever "mass gap" collision)</li> <li><a href="/w/index.php?title=GW200105&action=edit&redlink=1" class="new" title="GW200105 (page does not exist)">GW200105</a> (first black hole - neutron star merger)</li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Methods</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li>Direct detection <ul><li><a href="/wiki/Interferometric_gravitational-wave_detector" class="mw-redirect" title="Interferometric gravitational-wave detector">Laser interferometers</a></li> <li>Resonant mass detectors</li> <li><i>Proposed: <a href="/wiki/Atom_interferometer" title="Atom interferometer">Atom interferometers</a></i></li></ul></li> <li>Indirect detection <ul><li><a href="/wiki/Cosmic_microwave_background#B-modes" title="Cosmic microwave background">B-modes</a> of <a href="/wiki/Cosmic_microwave_background" title="Cosmic microwave background">CMB</a></li> <li><a href="/wiki/Pulsar_timing_array" title="Pulsar timing array">Pulsar timing array</a></li> <li><a href="/wiki/Binary_pulsar" title="Binary pulsar">Binary pulsar</a></li></ul></li></ul> </div></td></tr></tbody></table><div></div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Theory</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/General_relativity" title="General relativity">General relativity</a></li> <li><a href="/wiki/Tests_of_general_relativity" title="Tests of general relativity">Tests of general relativity</a></li> <li><a href="/wiki/Alternatives_to_general_relativity" title="Alternatives to general relativity">Metric theories</a></li> <li><a href="/wiki/Graviton" title="Graviton">Graviton</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Effects / properties</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Gravitational_wave#Effects_of_passing" title="Gravitational wave">Polarization</a></li> <li><a href="/wiki/Spin-flip" title="Spin-flip">Spin-flip</a></li> <li><a href="/wiki/Redshift" title="Redshift">Redshift</a></li> <li>Travel with <a href="/wiki/Speed_of_light" title="Speed of light">speed of light</a></li> <li>h strain</li> <li>Chirp signal (<a href="/wiki/Chirp_mass" title="Chirp mass">chirp mass</a>)</li> <li>Carried <a href="/wiki/Energy" title="Energy">energy</a></li> <li><a href="/wiki/Gravitational_wave_background" title="Gravitational wave background">Gravitational wave background</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Types / sources</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Stochastic" title="Stochastic">Stochastic</a> <ul><li><a href="/wiki/Cosmic_inflation" title="Cosmic inflation">Cosmic inflation</a>-<a href="/wiki/Quantum_fluctuation" title="Quantum fluctuation">quantum fluctuation</a></li> <li><a href="/wiki/Phase_transition" title="Phase transition">Phase transition</a></li></ul></li> <li>Binary inspiral <ul><li><a href="/wiki/Supermassive_black_hole" title="Supermassive black hole">Supermassive black holes</a></li> <li><a href="/wiki/Stellar_black_hole" title="Stellar black hole">Stellar black holes</a></li> <li><a class="mw-selflink selflink">Neutron stars</a></li> <li><a href="/wiki/Extreme_mass_ratio_inspiral" title="Extreme mass ratio inspiral">EMRI</a></li></ul></li> <li>Continuous <ul><li>Rotating neutron star</li></ul></li> <li>Burst <ul><li><a href="/wiki/Supernova" title="Supernova">Supernova</a> or from <i>unknown</i> sources</li></ul></li> <li>Hypothesis <ul><li>Colliding <a href="/wiki/Cosmic_string" title="Cosmic string">cosmic string</a> and <i>other unknown</i> sources</li></ul></li></ul> </div></td></tr></tbody></table></div> <style data-mw-deduplicate="TemplateStyles:r1130092004">.mw-parser-output .portal-bar{font-size:88%;font-weight:bold;display:flex;justify-content:center;align-items:baseline}.mw-parser-output .portal-bar-bordered{padding:0 2em;background-color:#fdfdfd;border:1px solid #a2a9b1;clear:both;margin:1em auto 0}.mw-parser-output .portal-bar-related{font-size:100%;justify-content:flex-start}.mw-parser-output .portal-bar-unbordered{padding:0 1.7em;margin-left:0}.mw-parser-output .portal-bar-header{margin:0 1em 0 0.5em;flex:0 0 auto;min-height:24px}.mw-parser-output .portal-bar-content{display:flex;flex-flow:row wrap;flex:0 1 auto;padding:0.15em 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.navbox+style+.portal-bar-bordered,.mw-parser-output .sister-bar+link+.portal-bar,.mw-parser-output .sister-bar+style+.portal-bar,.mw-parser-output .portal-bar+.navbox-styles+.navbox,.mw-parser-output .portal-bar+.navbox-styles+.sister-bar{margin-top:-1px}</style><div class="portal-bar noprint metadata noviewer portal-bar-bordered" role="navigation" aria-label="Portals"><span class="portal-bar-header"><a href="/wiki/Wikipedia:Contents/Portals" title="Wikipedia:Contents/Portals">Portals</a>:</span><ul class="portal-bar-content"><li class="portal-bar-item"><span class="nowrap"><span typeof="mw:File"><span><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/0/00/Crab_Nebula.jpg/19px-Crab_Nebula.jpg" decoding="async" width="19" height="19" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/0/00/Crab_Nebula.jpg/29px-Crab_Nebula.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/0/00/Crab_Nebula.jpg/38px-Crab_Nebula.jpg 2x" data-file-width="3864" 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