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class="vector-toc-text"> <span class="vector-toc-numb">2</span> <span>Use of kinematic measurements</span> </div> </a> <ul id="toc-Use_of_kinematic_measurements-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Recent_advancements_due_to_Gaia" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#Recent_advancements_due_to_Gaia"> <div class="vector-toc-text"> <span class="vector-toc-numb">3</span> <span>Recent advancements due to <i>Gaia</i></span> </div> </a> <ul id="toc-Recent_advancements_due_to_Gaia-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Stellar_kinematic_types" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#Stellar_kinematic_types"> <div class="vector-toc-text"> <span class="vector-toc-numb">4</span> <span>Stellar kinematic types</span> </div> </a> <button aria-controls="toc-Stellar_kinematic_types-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 Stellar kinematic types subsection</span> </button> <ul id="toc-Stellar_kinematic_types-sublist" class="vector-toc-list"> <li id="toc-High-velocity_stars" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#High-velocity_stars"> <div class="vector-toc-text"> <span class="vector-toc-numb">4.1</span> <span>High-velocity stars</span> </div> </a> <ul id="toc-High-velocity_stars-sublist" class="vector-toc-list"> <li id="toc-Runaway_stars" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Runaway_stars"> <div class="vector-toc-text"> <span class="vector-toc-numb">4.1.1</span> <span>Runaway stars</span> </div> </a> <ul id="toc-Runaway_stars-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Halo_stars" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Halo_stars"> <div class="vector-toc-text"> <span class="vector-toc-numb">4.1.2</span> <span>Halo stars</span> </div> </a> <ul id="toc-Halo_stars-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Hypervelocity_stars" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Hypervelocity_stars"> <div class="vector-toc-text"> <span class="vector-toc-numb">4.1.3</span> <span>Hypervelocity stars</span> </div> </a> <ul id="toc-Hypervelocity_stars-sublist" class="vector-toc-list"> <li id="toc-Origin_of_hypervelocity_stars" class="vector-toc-list-item vector-toc-level-4"> <a class="vector-toc-link" href="#Origin_of_hypervelocity_stars"> <div class="vector-toc-text"> <span class="vector-toc-numb">4.1.3.1</span> <span>Origin of hypervelocity stars</span> </div> </a> <ul id="toc-Origin_of_hypervelocity_stars-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Partial_list_of_HVSs" class="vector-toc-list-item vector-toc-level-4"> <a class="vector-toc-link" href="#Partial_list_of_HVSs"> <div class="vector-toc-text"> <span class="vector-toc-numb">4.1.3.2</span> <span>Partial list of HVSs</span> </div> </a> <ul id="toc-Partial_list_of_HVSs-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> </ul> </li> </ul> </li> <li id="toc-Kinematic_groups" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#Kinematic_groups"> <div class="vector-toc-text"> <span class="vector-toc-numb">5</span> <span>Kinematic groups</span> </div> </a> <button aria-controls="toc-Kinematic_groups-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 Kinematic groups subsection</span> </button> <ul id="toc-Kinematic_groups-sublist" class="vector-toc-list"> <li id="toc-Stellar_associations" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Stellar_associations"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.1</span> <span>Stellar associations</span> </div> </a> <ul id="toc-Stellar_associations-sublist" class="vector-toc-list"> <li id="toc-Types" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#Types"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.1.1</span> <span>Types</span> </div> </a> <ul id="toc-Types-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-OB_associations" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#OB_associations"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.1.2</span> <span>OB associations</span> </div> </a> <ul id="toc-OB_associations-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-T_associations" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#T_associations"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.1.3</span> <span>T associations</span> </div> </a> <ul id="toc-T_associations-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-R_associations" class="vector-toc-list-item vector-toc-level-3"> <a class="vector-toc-link" href="#R_associations"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.1.4</span> <span>R associations</span> </div> </a> <ul id="toc-R_associations-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Moving_groups" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Moving_groups"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.2</span> <span>Moving groups</span> </div> </a> <ul id="toc-Moving_groups-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Stellar_streams" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Stellar_streams"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.3</span> <span>Stellar streams</span> </div> </a> <ul id="toc-Stellar_streams-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Known_kinematic_groups" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Known_kinematic_groups"> <div class="vector-toc-text"> <span class="vector-toc-numb">5.4</span> <span>Known kinematic groups</span> </div> </a> <ul id="toc-Known_kinematic_groups-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-See_also" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#See_also"> <div class="vector-toc-text"> <span class="vector-toc-numb">6</span> <span>See also</span> </div> </a> <ul id="toc-See_also-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-References" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#References"> <div class="vector-toc-text"> <span class="vector-toc-numb">7</span> <span>References</span> </div> </a> <ul id="toc-References-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Further_reading" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#Further_reading"> <div class="vector-toc-text"> <span class="vector-toc-numb">8</span> <span>Further reading</span> </div> </a> <ul id="toc-Further_reading-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-External_links" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#External_links"> <div class="vector-toc-text"> <span class="vector-toc-numb">9</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" 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mw-first-heading"><span class="mw-page-title-main">Stellar kinematics</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 25 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-25" 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">25 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/Sterkinematika" title="Sterkinematika – Afrikaans" lang="af" hreflang="af" data-title="Sterkinematika" data-language-autonym="Afrikaans" data-language-local-name="Afrikaans" class="interlanguage-link-target"><span>Afrikaans</span></a></li><li class="interlanguage-link interwiki-ar mw-list-item"><a href="https://ar.wikipedia.org/wiki/%D8%B9%D9%84%D9%85_%D8%AD%D8%B1%D9%83%D8%A9_%D8%A7%D9%84%D9%86%D8%AC%D9%88%D9%85_%D8%A7%D9%84%D9%85%D8%AC%D8%B1%D8%AF%D8%A9" title="علم حركة النجوم المجردة – Arabic" lang="ar" hreflang="ar" data-title="علم حركة النجوم المجردة" data-language-autonym="العربية" data-language-local-name="Arabic" class="interlanguage-link-target"><span>العربية</span></a></li><li class="interlanguage-link interwiki-ca mw-list-item"><a href="https://ca.wikipedia.org/wiki/Cinem%C3%A0tica_estel%C2%B7lar" title="Cinemàtica estel·lar – Catalan" lang="ca" hreflang="ca" data-title="Cinemàtica estel·lar" data-language-autonym="Català" data-language-local-name="Catalan" class="interlanguage-link-target"><span>Català</span></a></li><li class="interlanguage-link interwiki-es mw-list-item"><a href="https://es.wikipedia.org/wiki/Cinem%C3%A1tica_estelar" title="Cinemática estelar – Spanish" lang="es" hreflang="es" data-title="Cinemática estelar" data-language-autonym="Español" data-language-local-name="Spanish" class="interlanguage-link-target"><span>Español</span></a></li><li class="interlanguage-link interwiki-eu mw-list-item"><a href="https://eu.wikipedia.org/wiki/Izar-zinematika" title="Izar-zinematika – Basque" lang="eu" hreflang="eu" data-title="Izar-zinematika" 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%DB%8C%D9%86%D9%85%D8%A7%D8%AA%DB%8C%DA%A9_%D8%B3%D8%AA%D8%A7%D8%B1%D9%87%E2%80%8C%D8%A7%DB%8C" title="سینماتیک ستاره‌ای – Persian" lang="fa" hreflang="fa" data-title="سینماتیک ستاره‌ای" 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/Cin%C3%A9matique_stellaire" title="Cinématique stellaire – French" lang="fr" hreflang="fr" data-title="Cinématique stellaire" data-language-autonym="Français" data-language-local-name="French" class="interlanguage-link-target"><span>Français</span></a></li><li class="interlanguage-link interwiki-ko mw-list-item"><a href="https://ko.wikipedia.org/wiki/%ED%95%AD%EC%84%B1%EC%9A%B4%EB%8F%99%ED%95%99" title="항성운동학 – Korean" lang="ko" hreflang="ko" data-title="항성운동학" data-language-autonym="한국어" data-language-local-name="Korean" class="interlanguage-link-target"><span>한국어</span></a></li><li class="interlanguage-link interwiki-id mw-list-item"><a href="https://id.wikipedia.org/wiki/Kinematika_bintang" title="Kinematika bintang – Indonesian" lang="id" hreflang="id" data-title="Kinematika bintang" 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-it mw-list-item"><a href="https://it.wikipedia.org/wiki/Cinematica_stellare" title="Cinematica stellare – Italian" lang="it" hreflang="it" data-title="Cinematica stellare" data-language-autonym="Italiano" data-language-local-name="Italian" class="interlanguage-link-target"><span>Italiano</span></a></li><li class="interlanguage-link interwiki-ky mw-list-item"><a href="https://ky.wikipedia.org/wiki/%D0%96%D1%8B%D0%BB%D0%B4%D1%8B%D0%B7%D0%B4%D0%B0%D1%80%D0%B4%D1%8B%D0%BD_%D0%BA%D1%8B%D0%B9%D0%BC%D1%8B%D0%BB%D1%8B" title="Жылдыздардын кыймылы – Kyrgyz" lang="ky" hreflang="ky" data-title="Жылдыздардын кыймылы" data-language-autonym="Кыргызча" data-language-local-name="Kyrgyz" class="interlanguage-link-target"><span>Кыргызча</span></a></li><li class="interlanguage-link interwiki-mk mw-list-item"><a href="https://mk.wikipedia.org/wiki/%D0%85%D0%B2%D0%B5%D0%B7%D0%B4%D0%B5%D0%BD%D0%B0_%D0%BA%D0%B8%D0%BD%D0%B5%D0%BC%D0%B0%D1%82%D0%B8%D0%BA%D0%B0" title="Ѕвездена кинематика – Macedonian" lang="mk" hreflang="mk" data-title="Ѕвездена кинематика" data-language-autonym="Македонски" data-language-local-name="Macedonian" class="interlanguage-link-target"><span>Македонски</span></a></li><li class="interlanguage-link interwiki-ms mw-list-item"><a href="https://ms.wikipedia.org/wiki/Kinematik_bintang" title="Kinematik bintang – Malay" lang="ms" hreflang="ms" data-title="Kinematik bintang" 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-ja mw-list-item"><a href="https://ja.wikipedia.org/wiki/%E9%81%8B%E5%8B%95%E6%98%9F%E5%9B%A3" title="運動星団 – Japanese" lang="ja" hreflang="ja" data-title="運動星団" 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/Stjernekinematikk" title="Stjernekinematikk – Norwegian Bokmål" lang="nb" hreflang="nb" data-title="Stjernekinematikk" 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/Stjerne-assosiasjon" title="Stjerne-assosiasjon – Norwegian Nynorsk" lang="nn" hreflang="nn" data-title="Stjerne-assosiasjon" 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-pt mw-list-item"><a href="https://pt.wikipedia.org/wiki/Cinem%C3%A1tica_estelar" title="Cinemática estelar – Portuguese" lang="pt" hreflang="pt" data-title="Cinemática estelar" 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/Cinematic%C4%83_stelar%C4%83" title="Cinematică stelară – Romanian" lang="ro" hreflang="ro" data-title="Cinematică stelară" 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%97%D0%B2%D1%91%D0%B7%D0%B4%D0%BD%D0%B0%D1%8F_%D0%BA%D0%B8%D0%BD%D0%B5%D0%BC%D0%B0%D1%82%D0%B8%D0%BA%D0%B0" title="Звёздная кинематика – Russian" lang="ru" hreflang="ru" data-title="Звёздная кинематика" data-language-autonym="Русский" data-language-local-name="Russian" class="interlanguage-link-target"><span>Русский</span></a></li><li class="interlanguage-link interwiki-sr mw-list-item"><a href="https://sr.wikipedia.org/wiki/Zvezdana_kinematika" title="Zvezdana kinematika – Serbian" lang="sr" hreflang="sr" data-title="Zvezdana kinematika" 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-fi mw-list-item"><a href="https://fi.wikipedia.org/wiki/Liikkuva_ryhm%C3%A4" title="Liikkuva ryhmä – Finnish" lang="fi" hreflang="fi" data-title="Liikkuva ryhmä" data-language-autonym="Suomi" data-language-local-name="Finnish" class="interlanguage-link-target"><span>Suomi</span></a></li><li class="interlanguage-link interwiki-th mw-list-item"><a href="https://th.wikipedia.org/wiki/%E0%B8%88%E0%B8%A5%E0%B8%99%E0%B8%A8%E0%B8%B2%E0%B8%AA%E0%B8%95%E0%B8%A3%E0%B9%8C%E0%B8%94%E0%B8%B2%E0%B8%A7%E0%B8%A4%E0%B8%81%E0%B8%A9%E0%B9%8C" title="จลนศาสตร์ดาวฤกษ์ – Thai" lang="th" hreflang="th" data-title="จลนศาสตร์ดาวฤกษ์" 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/Y%C4%B1ld%C4%B1z_kinemati%C4%9Fi" title="Yıldız kinematiği – Turkish" lang="tr" hreflang="tr" data-title="Yıldız kinematiği" 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%97%D0%BE%D1%80%D1%8F%D0%BD%D0%B0_%D0%BA%D1%96%D0%BD%D0%B5%D0%BC%D0%B0%D1%82%D0%B8%D0%BA%D0%B0" title="Зоряна кінематика – Ukrainian" lang="uk" hreflang="uk" data-title="Зоряна кінематика" data-language-autonym="Українська" data-language-local-name="Ukrainian" class="interlanguage-link-target"><span>Українська</span></a></li><li class="interlanguage-link interwiki-zh mw-list-item"><a href="https://zh.wikipedia.org/wiki/%E6%81%86%E6%98%9F%E9%81%8B%E5%8B%95%E5%AD%B8" title="恆星運動學 – Chinese" lang="zh" hreflang="zh" data-title="恆星運動學" data-language-autonym="中文" data-language-local-name="Chinese" class="interlanguage-link-target"><span>中文</span></a></li> </ul> <div class="after-portlet after-portlet-lang"><span class="wb-langlinks-edit wb-langlinks-link"><a href="https://www.wikidata.org/wiki/Special:EntityPage/Q6440#sitelinks-wikipedia" title="Edit interlanguage links" class="wbc-editpage">Edit links</a></span></div> </div> </div> </div> </header> <div class="vector-page-toolbar"> <div class="vector-page-toolbar-container"> <div id="left-navigation"> <nav aria-label="Namespaces"> <div id="p-associated-pages" class="vector-menu vector-menu-tabs mw-portlet mw-portlet-associated-pages" > <div class="vector-menu-content"> <ul class="vector-menu-content-list"> <li id="ca-nstab-main" class="selected vector-tab-noicon mw-list-item"><a href="/wiki/Stellar_kinematics" title="View the content page [c]" accesskey="c"><span>Article</span></a></li><li id="ca-talk" class="vector-tab-noicon mw-list-item"><a href="/wiki/Talk:Stellar_kinematics" rel="discussion" title="Discuss improvements to 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id="siteSub" class="noprint">From Wikipedia, the free encyclopedia</div> </div> <div id="contentSub"><div id="mw-content-subtitle"></div></div> <div id="mw-content-text" class="mw-body-content"><div class="mw-content-ltr mw-parser-output" lang="en" dir="ltr"><div class="shortdescription nomobile noexcerpt noprint searchaux" style="display:none">Study of the movement of stars</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">"Space velocity (astronomy)" redirects here. Not to be confused with <a href="/wiki/Radial_velocity" title="Radial velocity">radial velocity</a>, <a href="/wiki/Proper_motion" title="Proper motion">proper motion</a>, or <a href="/wiki/Peculiar_velocity" title="Peculiar velocity">peculiar velocity</a>.</div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Barnard2005.gif" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/6/6c/Barnard2005.gif/220px-Barnard2005.gif" decoding="async" width="220" height="195" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/6/6c/Barnard2005.gif 1.5x" data-file-width="308" data-file-height="273" /></a><figcaption><a href="/wiki/Barnard%27s_Star" title="Barnard's Star">Barnard's Star</a>, showing position every 5 years in the period 1985–2005. Barnard's Star is the star with the highest <a href="/wiki/Proper_motion" title="Proper motion">proper motion</a>.<sup id="cite_ref-Kaler_1-0" class="reference"><a href="#cite_note-Kaler-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup></figcaption></figure> <p>In <a href="/wiki/Astronomy" title="Astronomy">astronomy</a>, <b>stellar kinematics</b> is the <a href="/wiki/Observational_astronomy" title="Observational astronomy">observational</a> study or measurement of the <a href="/wiki/Kinematics" title="Kinematics">kinematics</a> or motions of <a href="/wiki/Star" title="Star">stars</a> through space. </p><p>Stellar kinematics encompasses the measurement of stellar <a href="/wiki/Velocity" title="Velocity">velocities</a> in the <a href="/wiki/Milky_Way" title="Milky Way">Milky Way</a> and its <a href="/wiki/Satellite_galaxies_of_the_Milky_Way" title="Satellite galaxies of the Milky Way">satellites</a> as well as the internal kinematics of more distant <a href="/wiki/Galaxy" title="Galaxy">galaxies</a>. Measurement of the kinematics of stars in different subcomponents of the Milky Way including the <a href="/wiki/Thin_disk" title="Thin disk">thin disk</a>, the <a href="/wiki/Thick_disk" title="Thick disk">thick disk</a>, the <a href="/wiki/Bulge_(astronomy)" class="mw-redirect" title="Bulge (astronomy)">bulge</a>, and the <a href="/wiki/Stellar_halo" title="Stellar halo">stellar halo</a> provides important information about the formation and evolutionary history of our Galaxy. Kinematic measurements can also identify exotic phenomena such as hypervelocity stars escaping from the Milky Way, which are interpreted as the result of gravitational encounters of <a href="/wiki/Binary_star" title="Binary star">binary stars</a> with the <a href="/wiki/Sagittarius_A*" title="Sagittarius A*">supermassive black hole at the Galactic Center</a>. </p><p>Stellar kinematics is related to but distinct from the subject of <a href="/wiki/Stellar_dynamics" title="Stellar dynamics">stellar dynamics</a>, which involves the theoretical study or modeling of the motions of stars under the influence of <a href="/wiki/Gravity" title="Gravity">gravity</a>. Stellar-dynamical models of systems such as galaxies or star clusters are often compared with or tested against stellar-kinematic data to study their evolutionary history and mass distributions, and to detect the presence of <a href="/wiki/Dark_matter" title="Dark matter">dark matter</a> or <a href="/wiki/Supermassive_black_hole" title="Supermassive black hole">supermassive black holes</a> through their gravitational influence on stellar orbits. </p> <meta property="mw:PageProp/toc" /> <div class="mw-heading mw-heading2"><h2 id="Space_velocity">Space velocity</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=1" title="Edit section: Space velocity"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure typeof="mw:File/Thumb"><a href="/wiki/File:Proper_motion.JPG" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/f/f2/Proper_motion.JPG/250px-Proper_motion.JPG" decoding="async" width="250" height="157" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/f/f2/Proper_motion.JPG/375px-Proper_motion.JPG 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/f/f2/Proper_motion.JPG/500px-Proper_motion.JPG 2x" data-file-width="964" data-file-height="606" /></a><figcaption>Relation between proper motion and velocity components of an object. At emission, the object was at distance <i>d</i> from the Sun, and moved at angular rate <i>μ</i> radian/s, that is, <i>μ = v<sub>t</sub> / d</i> with <i>v<sub>t</sub></i> = the component of velocity transverse to line of sight from the Sun. (The diagram illustrates an angle <i>μ</i> swept out in unit time at tangential velocity <i>v<sub>t</sub></i>.)</figcaption></figure> <p>The component of stellar motion toward or away from the Sun, known as <a href="/wiki/Radial_velocity" title="Radial velocity">radial velocity</a>, can be measured from the spectrum shift caused by the <a href="/wiki/Doppler_effect" title="Doppler effect">Doppler effect</a>. The transverse, or <a href="/wiki/Proper_motion" title="Proper motion">proper motion</a> must be found by taking a series of positional determinations against more distant objects. Once the distance to a star is determined through <a href="/wiki/Astrometric" class="mw-redirect" title="Astrometric">astrometric</a> means such as <a href="/wiki/Parallax" title="Parallax">parallax</a>, the space velocity can be computed.<sup id="cite_ref-atoe05_2-0" class="reference"><a href="#cite_note-atoe05-2"><span class="cite-bracket">[</span>2<span class="cite-bracket">]</span></a></sup> This is the star's <i>actual motion</i> relative to the <a href="/wiki/Sun" title="Sun">Sun</a> or the <a href="/wiki/Local_standard_of_rest" title="Local standard of rest">local standard of rest</a> (LSR). The latter is typically taken as a position at the Sun's present location that is following a circular orbit around the <a href="/wiki/Galactic_Center" title="Galactic Center">Galactic Center</a> at the mean velocity of those nearby stars with low velocity dispersion.<sup id="cite_ref-araa29_3-0" class="reference"><a href="#cite_note-araa29-3"><span class="cite-bracket">[</span>3<span class="cite-bracket">]</span></a></sup> The Sun's motion with respect to the LSR is called the "peculiar solar motion". </p><p>The components of space velocity in the <a href="/wiki/Milky_Way" title="Milky Way">Milky Way</a>'s <a href="/wiki/Galactic_coordinate_system" title="Galactic coordinate system">Galactic coordinate system</a> are usually designated U, V, and W, given in km/s, with U positive in the direction of the Galactic Center, V positive in the direction of <a href="/wiki/Milky_Way#Galactic_rotation" title="Milky Way">galactic rotation</a>, and W positive in the direction of the <a href="/wiki/North_Galactic_Pole" class="mw-redirect" title="North Galactic Pole">North Galactic Pole</a>.<sup id="cite_ref-aj93_2_4-0" class="reference"><a href="#cite_note-aj93_2-4"><span class="cite-bracket">[</span>4<span class="cite-bracket">]</span></a></sup> The peculiar motion of the Sun with respect to the LSR is<sup id="cite_ref-mnras403_5-0" class="reference"><a href="#cite_note-mnras403-5"><span class="cite-bracket">[</span>5<span class="cite-bracket">]</span></a></sup> </p> <dl><dd>(U, V, W) = (11.1, 12.24, 7.25) km/s,</dd></dl> <p>with statistical uncertainty (+0.69−0.75, +0.47−0.47, +0.37−0.36) km/s and systematic uncertainty (1, 2, 0.5) km/s. (Note that V is 7 km/s larger than estimated in 1998 by Dehnen et al.<sup id="cite_ref-mnras298_6-0" class="reference"><a href="#cite_note-mnras298-6"><span class="cite-bracket">[</span>6<span class="cite-bracket">]</span></a></sup>) </p> <div class="mw-heading mw-heading2"><h2 id="Use_of_kinematic_measurements">Use of kinematic measurements</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=2" title="Edit section: Use of kinematic measurements"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Stellar kinematics yields important <a href="/wiki/Astrophysics" title="Astrophysics">astrophysical</a> information about stars, and the galaxies in which they reside. Stellar kinematics data combined with astrophysical modeling produces important information about the galactic system as a whole. Measured stellar velocities in the innermost regions of galaxies including the Milky Way have provided evidence that many galaxies host <a href="/wiki/Supermassive_black_hole" title="Supermassive black hole">supermassive black holes</a> at their center. In farther out regions of galaxies such as within the galactic halo, velocity measurements of <a href="/wiki/Globular_cluster" title="Globular cluster">globular</a> clusters orbiting in these halo regions of galaxies provides evidence for <a href="/wiki/Dark_matter" title="Dark matter">dark matter</a>. Both of these cases derive from the key fact that stellar kinematics can be related to the overall <a href="/wiki/Gravitational_potential" title="Gravitational potential">potential</a> in which the stars are bound. This means that if accurate stellar kinematics measurements are made for a star or group of stars orbiting in a certain region of a galaxy, the gravitational potential and mass distribution can be inferred given that the gravitational potential in which the star is bound produces its orbit and serves as the impetus for its stellar motion. Examples of using kinematics combined with modeling to construct an astrophysical system include: </p> <ul><li><b>Rotation of the Milky Way's disc</b>: From the <a href="/wiki/Proper_motion" title="Proper motion">proper motions</a> and <a href="/wiki/Radial_velocities" class="mw-redirect" title="Radial velocities">radial velocities</a> of stars within the Milky way disc one can show that there is differential rotation. When combining these measurements of stars' proper motions and their radial velocities, along with careful modeling, it is possible to obtain a picture of the rotation of the Milky Way <a href="/wiki/Disc_galaxy" title="Disc galaxy">disc</a>. The local character of galactic rotation in the <a href="/wiki/Solar_neighborhood" class="mw-redirect" title="Solar neighborhood">solar neighborhood</a> is encapsulated in the <a href="/wiki/Oort_constants" title="Oort constants">Oort constants</a>.<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><sup id="cite_ref-8" class="reference"><a href="#cite_note-8"><span class="cite-bracket">[</span>8<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-9" class="reference"><a href="#cite_note-9"><span class="cite-bracket">[</span>9<span class="cite-bracket">]</span></a></sup></li> <li><b>Structural components of the Milky Way</b>: Using stellar kinematics, astronomers construct models which seek to explain the overall galactic structure in terms of distinct kinematic populations of stars. This is possible because these distinct populations are often located in specific regions of galaxies. For example, within the <a href="/wiki/Milky_Way" title="Milky Way">Milky Way</a>, there are three primary components, each with its own distinct stellar kinematics: the <a href="/wiki/Galactic_Disc" class="mw-redirect" title="Galactic Disc">disc</a>, <a href="/wiki/Milky_Way_halo" class="mw-redirect" title="Milky Way halo">halo</a> and <a href="/wiki/Bulge_(astronomy)" class="mw-redirect" title="Bulge (astronomy)">bulge or bar</a>. These kinematic groups are closely related to the stellar populations in the Milky Way, forming a strong correlation between the motion and chemical composition, thus indicating different formation mechanisms. For the Milky Way, the speed of disk stars is <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 \mathrm {V} =220~\mathrm {km} ~\mathrm {s} ^{-1}}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mrow class="MJX-TeXAtom-ORD"> <mi mathvariant="normal">V</mi> </mrow> <mo>=</mo> <mn>220</mn> <mtext> </mtext> <mrow class="MJX-TeXAtom-ORD"> <mi mathvariant="normal">k</mi> <mi mathvariant="normal">m</mi> </mrow> <mtext> </mtext> <msup> <mrow class="MJX-TeXAtom-ORD"> <mi mathvariant="normal">s</mi> </mrow> <mrow class="MJX-TeXAtom-ORD"> <mo>−</mo> <mn>1</mn> </mrow> </msup> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle \mathrm {V} =220~\mathrm {km} ~\mathrm {s} ^{-1}}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/a413235b4bb679b971d93483503a220205d38916" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.338ex; width:15.903ex; height:2.676ex;" alt="{\displaystyle \mathrm {V} =220~\mathrm {km} ~\mathrm {s} ^{-1}}"></span> and an RMS (<a href="/wiki/Root_mean_square" title="Root mean square">Root mean square</a>) velocity relative to this speed of <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 \mathrm {V_{RMS}} =50~\mathrm {km} ~\mathrm {s} ^{-1}}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mrow class="MJX-TeXAtom-ORD"> <msub> <mi mathvariant="normal">V</mi> <mrow class="MJX-TeXAtom-ORD"> <mi mathvariant="normal">R</mi> <mi mathvariant="normal">M</mi> <mi mathvariant="normal">S</mi> </mrow> </msub> </mrow> <mo>=</mo> <mn>50</mn> <mtext> </mtext> <mrow class="MJX-TeXAtom-ORD"> <mi mathvariant="normal">k</mi> <mi mathvariant="normal">m</mi> </mrow> <mtext> </mtext> <msup> <mrow class="MJX-TeXAtom-ORD"> <mi mathvariant="normal">s</mi> </mrow> <mrow class="MJX-TeXAtom-ORD"> <mo>−</mo> <mn>1</mn> </mrow> </msup> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle \mathrm {V_{RMS}} =50~\mathrm {km} ~\mathrm {s} ^{-1}}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/bc4ef5ffe32e6ead0f795885ee07c5749e097b39" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.671ex; width:18.603ex; height:3.009ex;" alt="{\displaystyle \mathrm {V_{RMS}} =50~\mathrm {km} ~\mathrm {s} ^{-1}}"></span>. For bulge population stars, the velocities are randomly oriented with a larger relative RMS velocity of <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 \mathrm {V_{RMS}} =150~\mathrm {km} ~\mathrm {s} ^{-1}}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mrow class="MJX-TeXAtom-ORD"> <msub> <mi mathvariant="normal">V</mi> <mrow class="MJX-TeXAtom-ORD"> <mi mathvariant="normal">R</mi> <mi mathvariant="normal">M</mi> <mi mathvariant="normal">S</mi> </mrow> </msub> </mrow> <mo>=</mo> <mn>150</mn> <mtext> </mtext> <mrow class="MJX-TeXAtom-ORD"> <mi mathvariant="normal">k</mi> <mi mathvariant="normal">m</mi> </mrow> <mtext> </mtext> <msup> <mrow class="MJX-TeXAtom-ORD"> <mi mathvariant="normal">s</mi> </mrow> <mrow class="MJX-TeXAtom-ORD"> <mo>−</mo> <mn>1</mn> </mrow> </msup> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle \mathrm {V_{RMS}} =150~\mathrm {km} ~\mathrm {s} ^{-1}}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/392feb4e0a018908aab3f26bcf6cad0ca8234f5a" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.671ex; width:19.765ex; height:3.009ex;" alt="{\displaystyle \mathrm {V_{RMS}} =150~\mathrm {km} ~\mathrm {s} ^{-1}}"></span> and no net circular velocity.<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> The Galactic stellar halo consists of stars with orbits that extend to the outer regions of the galaxy. Some of these stars will continually orbit far from the galactic center, while others are on trajectories which bring them to various distances from the galactic center. These stars have little to no average rotation. Many stars in this group belong to globular clusters which formed long ago and thus have a distinct formation history, which can be inferred from their kinematics and poor metallicities. The halo may be further subdivided into an inner and outer halo, with the inner halo having a net prograde motion with respect to the Milky Way and the outer a net <a href="/wiki/Retrograde_and_prograde_motion" title="Retrograde and prograde motion">retrograde motion</a>.<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></li> <li><b>External galaxies</b>: Spectroscopic observations of external galaxies make it possible to characterize the bulk motions of the stars they contain. While these stellar populations in external galaxies are generally not resolved to the level where one can track the motion of individual stars (except for the very nearest galaxies) measurements of the kinematics of the integrated stellar population along the line of sight provides information including the mean velocity and the <a href="/wiki/Velocity_dispersion" title="Velocity dispersion">velocity dispersion</a> which can then be used to infer the distribution of mass within the galaxy. Measurement of the mean velocity as a function of position gives information on the galaxy's rotation, with distinct regions of the galaxy that are <a href="/wiki/Redshift" title="Redshift">redshifted</a> / <a href="/wiki/Blueshift" class="mw-redirect" title="Blueshift">blueshifted</a> in relation to the galaxy's <a href="/wiki/Recessional_velocity" title="Recessional velocity">systemic velocity</a>.</li> <li><b>Mass distributions</b>: Through measurement of the kinematics of tracer objects such as globular clusters and the orbits of nearby <a href="/wiki/Satellite_galaxy" title="Satellite galaxy">satellite dwarf galaxies</a>, we can determine the mass distribution of the Milky Way or other galaxies. This is accomplished by combining kinematic measurements with dynamical modeling.</li></ul> <div class="mw-heading mw-heading2"><h2 id="Recent_advancements_due_to_Gaia">Recent advancements due to <i>Gaia</i></h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=3" title="Edit section: Recent advancements due to Gaia"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure typeof="mw:File/Thumb"><a href="/wiki/File:Gaia%E2%80%99s_stellar_motion_for_the_next_400_thousand_years_ESA22358019.png" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/9/95/Gaia%E2%80%99s_stellar_motion_for_the_next_400_thousand_years_ESA22358019.png/250px-Gaia%E2%80%99s_stellar_motion_for_the_next_400_thousand_years_ESA22358019.png" decoding="async" width="250" height="141" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/9/95/Gaia%E2%80%99s_stellar_motion_for_the_next_400_thousand_years_ESA22358019.png/375px-Gaia%E2%80%99s_stellar_motion_for_the_next_400_thousand_years_ESA22358019.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/9/95/Gaia%E2%80%99s_stellar_motion_for_the_next_400_thousand_years_ESA22358019.png/500px-Gaia%E2%80%99s_stellar_motion_for_the_next_400_thousand_years_ESA22358019.png 2x" data-file-width="3840" data-file-height="2160" /></a><figcaption>Expected motion of 40,000 stars in the next 400 thousand years, as determined by Gaia EDR3</figcaption></figure> <p>In 2018, the <a href="/wiki/Gaia_(spacecraft)" title="Gaia (spacecraft)">Gaia</a> Data Release 2 (GAIA DR2) marked a significant advancement in stellar kinematics, offering a rich dataset of precise measurements. This release included detailed stellar kinematic and <a href="/wiki/Stellar_parallax" title="Stellar parallax">stellar parallax</a> data, contributing to a more nuanced understanding of the Milky Way's structure. Notably, it facilitated the determination of proper motions for numerous celestial objects, including the absolute proper motions of 75 <a href="/wiki/Globular_cluster" title="Globular cluster">globular clusters</a> situated at distances extending up to <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=21}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>G</mi> <mo>=</mo> <mn>21</mn> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle G=21}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/4b5fd6d60acde2b6b41abbb2bfd399b98f37158f" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.338ex; width:7.25ex; height:2.176ex;" alt="{\displaystyle G=21}"></span> and a bright limit of <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\approx }"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mi>G</mi> <mo>≈</mo> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle G\approx }</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/c27d41cee12f1bc3cfdf8cea7fa2cbd45d8e963f" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.338ex; width:4.28ex; height:2.176ex;" alt="{\displaystyle G\approx }"></span> <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 3}"> <semantics> <mrow class="MJX-TeXAtom-ORD"> <mstyle displaystyle="true" scriptlevel="0"> <mn>3</mn> </mstyle> </mrow> <annotation encoding="application/x-tex">{\displaystyle 3}</annotation> </semantics> </math></span><img src="https://wikimedia.org/api/rest_v1/media/math/render/svg/991e33c6e207b12546f15bdfee8b5726eafbbb2f" class="mwe-math-fallback-image-inline mw-invert skin-invert" aria-hidden="true" style="vertical-align: -0.338ex; width:1.162ex; height:2.176ex;" alt="{\displaystyle 3}"></span>.<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> Furthermore, Gaia's comprehensive dataset enabled the measurement of absolute proper motions in nearby <a href="/wiki/Dwarf_spheroidal_galaxy" title="Dwarf spheroidal galaxy">dwarf spheroidal galaxies</a>, serving as crucial indicators for understanding the mass distribution within the Milky Way.<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> GAIA DR3 improved the quality of previously published data by providing detailed astrophysical parameters.<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> While the complete GAIA DR4 is yet to be unveiled, the latest release offers enhanced insights into white dwarfs, <a href="/wiki/Hypervelocity_stars" class="mw-redirect" title="Hypervelocity stars">hypervelocity stars</a>, cosmological <a href="/wiki/Gravitational_lens" title="Gravitational lens">gravitational lensing</a>, and the merger history of the <a href="/wiki/Galaxy" title="Galaxy">Galaxy</a>.<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> </p> <div class="mw-heading mw-heading2"><h2 id="Stellar_kinematic_types">Stellar kinematic types</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=4" title="Edit section: Stellar kinematic types"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Stars within galaxies may be classified based on their kinematics. For example, the stars in the Milky Way can be subdivided into two general populations, based on their <a href="/wiki/Metallicity" title="Metallicity">metallicity</a>, or proportion of elements with atomic numbers higher than helium. Among nearby stars, it has been found that population I stars with higher metallicity are generally located in the stellar disk while older population II stars are in random orbits with little net rotation.<sup id="cite_ref-pasp69_406_16-0" class="reference"><a href="#cite_note-pasp69_406-16"><span class="cite-bracket">[</span>16<span class="cite-bracket">]</span></a></sup> The latter have elliptical orbits that are inclined to the plane of the Milky Way.<sup id="cite_ref-pasp69_406_16-1" class="reference"><a href="#cite_note-pasp69_406-16"><span class="cite-bracket">[</span>16<span class="cite-bracket">]</span></a></sup> Comparison of the kinematics of nearby stars has also led to the identification of <a href="/wiki/Stellar_association" title="Stellar association">stellar associations</a>. These are most likely groups of stars that share a common point of origin in giant molecular clouds.<sup id="cite_ref-AS1998_17-0" class="reference"><a href="#cite_note-AS1998-17"><span class="cite-bracket">[</span>17<span class="cite-bracket">]</span></a></sup> </p><p>There are many additional ways to classify stars based on their measured velocity components, and this provides detailed information about the nature of the star's formation time, its present location, and the general structure of the galaxy. As a star moves in a galaxy, the smoothed out gravitational potential of all the other stars and other mass within the galaxy plays a dominant role in determining the stellar motion.<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> Stellar kinematics can provide insights into the location of where the star formed within the galaxy. Measurements of an individual star's kinematics can identify stars that are peculiar outliers such as a high-velocity star moving much faster than its nearby neighbors. </p> <div class="mw-heading mw-heading3"><h3 id="High-velocity_stars">High-velocity stars</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=5" title="Edit section: High-velocity stars"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Depending on the definition, a high-<a href="/wiki/Velocity" title="Velocity">velocity</a> star is a star moving faster than 65 km/s to 100 km/s relative to the average motion of the other stars in the star's neighborhood. The velocity is also sometimes defined as <a href="/wiki/Supersonic_speed" title="Supersonic speed">supersonic</a> relative to the surrounding interstellar medium. The three types of high-velocity stars are: runaway stars, halo stars and hypervelocity stars. High-velocity stars were studied by Jan Oort, who used their kinematic data to predict that high-velocity stars have very little tangential velocity.<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> </p> <div class="mw-heading mw-heading4"><h4 id="Runaway_stars">Runaway stars</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=6" title="Edit section: Runaway 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:Hs-2009-03-a-web_print.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/4/4d/Hs-2009-03-a-web_print.jpg/220px-Hs-2009-03-a-web_print.jpg" decoding="async" width="220" height="238" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/4/4d/Hs-2009-03-a-web_print.jpg/330px-Hs-2009-03-a-web_print.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/4/4d/Hs-2009-03-a-web_print.jpg/440px-Hs-2009-03-a-web_print.jpg 2x" data-file-width="846" data-file-height="916" /></a><figcaption>Four runaway stars moving through regions of dense interstellar gas and creating bright bow waves and trailing tails of glowing gas. The stars in these NASA Hubble Space Telescope images are among 14 young runaway stars spotted by the Advanced Camera for Surveys between October 2005 and July 2006.</figcaption></figure> <p>A runaway star is one that is moving through space with an abnormally high <a href="/wiki/Velocity" title="Velocity">velocity</a> relative to the surrounding <a href="/wiki/Interstellar_medium" title="Interstellar medium">interstellar medium</a>. The <a href="/wiki/Proper_motion" title="Proper motion">proper motion</a> of a runaway star often points exactly away from a <a href="/wiki/Stellar_association" title="Stellar association">stellar association</a>, of which the star was formerly a member, before it was hurled out. </p><p>Mechanisms that may give rise to a runaway star include: </p> <ul><li>Gravitational interactions between stars in a <a href="/wiki/Stellar_system" class="mw-redirect" title="Stellar system">stellar system</a> can result in large accelerations of one or more of the involved stars. In some cases, stars may even be ejected.<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> This can occur in seemingly stable star systems of only three stars, as described in studies of the <a href="/wiki/Three-body_problem" title="Three-body problem">three-body problem</a> in gravitational theory.<sup id="cite_ref-21" class="reference"><a href="#cite_note-21"><span class="cite-bracket">[</span>21<span class="cite-bracket">]</span></a></sup></li> <li>A collision or close encounter between stellar systems, including galaxies, may result in the disruption of both systems, with some of the stars being accelerated to high velocities, or even ejected. A large-scale example is the gravitational interaction between the <a href="/wiki/Milky_Way" title="Milky Way">Milky Way</a> and the <a href="/wiki/Large_Magellanic_Cloud" title="Large Magellanic Cloud">Large Magellanic Cloud</a>.<sup id="cite_ref-22" class="reference"><a href="#cite_note-22"><span class="cite-bracket">[</span>22<span class="cite-bracket">]</span></a></sup></li> <li>A <a href="/wiki/Supernova" title="Supernova">supernova</a> explosion in a <a href="/wiki/Multiple_star" class="mw-redirect" title="Multiple star">multiple star</a> system can accelerate both the supernova remnant and remaining stars to high velocities.<sup id="cite_ref-23" class="reference"><a href="#cite_note-23"><span class="cite-bracket">[</span>23<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-24" class="reference"><a href="#cite_note-24"><span class="cite-bracket">[</span>24<span class="cite-bracket">]</span></a></sup></li></ul> <p>Multiple mechanisms may accelerate the same runaway star. For example, a massive star that was originally ejected due to gravitational interactions with its stellar neighbors may itself go supernova, producing a remnant with a velocity modulated by the supernova kick. If this supernova occurs in the very nearby vicinity of other stars, it is possible that it may produce more runaways in the process. </p><p>An example of a related set of runaway stars is the case of <a href="/wiki/AE_Aurigae" title="AE Aurigae">AE Aurigae</a>, <a href="/wiki/53_Arietis" title="53 Arietis">53 Arietis</a> and <a href="/wiki/Mu_Columbae" title="Mu Columbae">Mu Columbae</a>, all of which are moving away from each other at velocities of over 100 km/s (for comparison, the <a href="/wiki/Sun" title="Sun">Sun</a> moves through the Milky Way at about 20 km/s faster than the local average). Tracing their motions back, their paths intersect near to the <a href="/wiki/Orion_Nebula" title="Orion Nebula">Orion Nebula</a> about 2 million years ago. <a href="/wiki/Barnard%27s_Loop" title="Barnard's Loop">Barnard's Loop</a> is believed to be the remnant of the supernova that launched the other stars. </p><p>Another example is the X-ray object <a href="/wiki/Vela_X-1" title="Vela X-1">Vela X-1</a>, where photodigital techniques reveal the presence of a typical supersonic <a href="/wiki/Bow_shocks_in_astrophysics" class="mw-redirect" title="Bow shocks in astrophysics">bow shock hyperbola</a>. </p> <div class="mw-heading mw-heading4"><h4 id="Halo_stars">Halo stars</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=7" title="Edit section: Halo stars"><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/Galactic_halo" title="Galactic halo">Galactic halo</a></div> <p>Halo stars are very old stars that do not follow circular orbits around the center of the Milky Way within its disk. Instead, the halo stars travel in elliptical orbits, often inclined to the disk, which take them well above and below the plane of the Milky Way. Although their orbital velocities relative to the Milky Way may be no faster than disk stars, their different paths result in high relative velocities. </p><p>Typical examples are the halo stars passing through the disk of the Milky Way at steep angles. One of the nearest 45 stars, called <a href="/wiki/Kapteyn%27s_Star" title="Kapteyn's Star">Kapteyn's Star</a>, is an example of the high-velocity stars that lie near the Sun: Its observed radial velocity is −245 km/s, and the components of its space velocity are <span class="nowrap"><span class="texhtml mvar" style="font-style:italic;">u</span> = +19 km/s,</span> <span class="nowrap"><span class="texhtml mvar" style="font-style:italic;">v</span> = −288 km/s,</span> and <span class="nowrap"><span class="texhtml mvar" style="font-style:italic;">w</span> = −52 km/s.</span> </p> <div class="mw-heading mw-heading4"><h4 id="Hypervelocity_stars">Hypervelocity stars</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=8" title="Edit section: Hypervelocity 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:Sprinting_stars_in_the_Milky_Way_ESA400471.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/c/cb/Sprinting_stars_in_the_Milky_Way_ESA400471.jpg/220px-Sprinting_stars_in_the_Milky_Way_ESA400471.jpg" decoding="async" width="220" height="124" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/c/cb/Sprinting_stars_in_the_Milky_Way_ESA400471.jpg/330px-Sprinting_stars_in_the_Milky_Way_ESA400471.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/c/cb/Sprinting_stars_in_the_Milky_Way_ESA400471.jpg/440px-Sprinting_stars_in_the_Milky_Way_ESA400471.jpg 2x" data-file-width="5906" data-file-height="3322" /></a><figcaption>Positions and trajectories of 20 high-velocity stars as reconstructed from data acquired by <i><a href="/wiki/Gaia_(spacecraft)" title="Gaia (spacecraft)">Gaia</a></i>, overlaid on top of an artistic view of the Milky Way</figcaption></figure> <p>Hypervelocity stars (designated as <b>HVS</b> or <b>HV</b> in stellar catalogues) have substantially higher velocities than the rest of the stellar population of a galaxy. Some of these stars may even exceed the <a href="/wiki/Escape_velocity" title="Escape velocity">escape velocity</a> of the galaxy.<sup id="cite_ref-25" class="reference"><a href="#cite_note-25"><span class="cite-bracket">[</span>25<span class="cite-bracket">]</span></a></sup> In the Milky Way, stars usually have velocities on the order of 100 km/s, whereas hypervelocity stars typically have velocities on the order of 1000 km/s. Most of these fast-moving stars are thought to be produced near the center of the Milky Way, where there is a larger population of these objects than further out. One of the fastest known stars in our Galaxy is the O-class sub-dwarf <a href="/wiki/US_708" title="US 708">US 708</a>, which is moving away from the Milky Way with a total velocity of around 1200 km/s. </p><p><a href="/wiki/Jack_G._Hills" title="Jack G. Hills">Jack G. Hills</a> first predicted the existence of HVSs in 1988.<sup id="cite_ref-26" class="reference"><a href="#cite_note-26"><span class="cite-bracket">[</span>26<span class="cite-bracket">]</span></a></sup> This was later confirmed in 2005 by Warren Brown, <a href="/wiki/Margaret_Geller" title="Margaret Geller">Margaret Geller</a>, <a href="/w/index.php?title=Scott_Kenyon&action=edit&redlink=1" class="new" title="Scott Kenyon (page does not exist)">Scott Kenyon</a>, and <a href="/wiki/Michael_J._Kurtz" title="Michael J. Kurtz">Michael Kurtz</a>.<sup id="cite_ref-HVS1_27-0" class="reference"><a href="#cite_note-HVS1-27"><span class="cite-bracket">[</span>27<span class="cite-bracket">]</span></a></sup> As of 2008,<sup class="plainlinks noexcerpt noprint asof-tag update" style="display:none;"><a class="external text" href="https://en.wikipedia.org/w/index.php?title=Stellar_kinematics&action=edit">[update]</a></sup> 10 <a href="/wiki/Intergalactic_star" title="Intergalactic star">unbound HVSs</a> were known, one of which is believed to have originated from the <a href="/wiki/Large_Magellanic_Cloud" title="Large Magellanic Cloud">Large Magellanic Cloud</a> rather than the <a href="/wiki/Milky_Way" title="Milky Way">Milky Way</a>.<sup id="cite_ref-HVS3_28-0" class="reference"><a href="#cite_note-HVS3-28"><span class="cite-bracket">[</span>28<span class="cite-bracket">]</span></a></sup> Further measurements placed its origin within the Milky Way.<sup id="cite_ref-Brown_29-0" class="reference"><a href="#cite_note-Brown-29"><span class="cite-bracket">[</span>29<span class="cite-bracket">]</span></a></sup> Due to uncertainty about the distribution of mass within the Milky Way, determining whether a HVS is unbound is difficult. A further five known high-velocity stars may be unbound from the Milky Way, and 16 HVSs are thought to be bound. The nearest currently known HVS (HVS2) is about 19 <a href="/wiki/Parsec" title="Parsec">kpc</a> from the Sun. </p><p>As of 1 September 2017<sup class="plainlinks noexcerpt noprint asof-tag update" style="display:none;"><a class="external text" href="https://en.wikipedia.org/w/index.php?title=Stellar_kinematics&action=edit">[update]</a></sup>, there have been roughly 20 observed hypervelocity stars. Though most of these were observed in the <a href="/wiki/Northern_Hemisphere" title="Northern Hemisphere">Northern Hemisphere</a>, the possibility remains that there are HVSs only observable from the <a href="/wiki/Southern_Hemisphere" title="Southern Hemisphere">Southern Hemisphere</a>.<sup id="cite_ref-30" class="reference"><a href="#cite_note-30"><span class="cite-bracket">[</span>30<span class="cite-bracket">]</span></a></sup> </p><p>It is believed that about 1,000 HVSs exist in the Milky Way.<sup id="cite_ref-apj671_2_1708_31-0" class="reference"><a href="#cite_note-apj671_2_1708-31"><span class="cite-bracket">[</span>31<span class="cite-bracket">]</span></a></sup> Considering that there are around 100 billion stars in the <a href="/wiki/Milky_Way" title="Milky Way">Milky Way</a>, this is a minuscule fraction (~0.000001%). Results from the second data release of <a href="/wiki/Gaia_(spacecraft)" title="Gaia (spacecraft)"><i>Gaia</i></a> (DR2) show that most high-velocity late-type stars have a high probability of being bound to the Milky Way.<sup id="cite_ref-32" class="reference"><a href="#cite_note-32"><span class="cite-bracket">[</span>32<span class="cite-bracket">]</span></a></sup> However, distant hypervelocity star candidates are more promising.<sup id="cite_ref-farfast_33-0" class="reference"><a href="#cite_note-farfast-33"><span class="cite-bracket">[</span>33<span class="cite-bracket">]</span></a></sup> </p><p>In March 2019, <a href="/w/index.php?title=LAMOST-HVS1&action=edit&redlink=1" class="new" title="LAMOST-HVS1 (page does not exist)">LAMOST-HVS1</a> was reported to be a confirmed hypervelocity star ejected from the stellar disk of the Milky Way.<sup id="cite_ref-PHYS-20190313_34-0" class="reference"><a href="#cite_note-PHYS-20190313-34"><span class="cite-bracket">[</span>34<span class="cite-bracket">]</span></a></sup> </p><p>In July 2019, astronomers reported finding an A-type star, <a href="/wiki/S5-HVS1" title="S5-HVS1">S5-HVS1</a>, traveling 1,755 km/s (3,930,000 mph), faster than any other star detected so far. The star is in the <a href="/wiki/Grus_(constellation)" title="Grus (constellation)">Grus</a> (or Crane) <a href="/wiki/Constellation" title="Constellation">constellation</a> in the southern sky and is about 29,000 ly (1.8<span style="margin:0 .15em 0 .25em">×</span>10<sup>9</sup> AU) from Earth. It may have been ejected from the Milky Way after interacting with <a href="/wiki/Sagittarius_A*" title="Sagittarius A*">Sagittarius A*</a>, the <a href="/wiki/Supermassive_black_hole" title="Supermassive black hole">supermassive black hole</a> at the center of the galaxy.<sup id="cite_ref-NYT-20191114_35-0" class="reference"><a href="#cite_note-NYT-20191114-35"><span class="cite-bracket">[</span>35<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-MNRAS-20191109_36-0" class="reference"><a href="#cite_note-MNRAS-20191109-36"><span class="cite-bracket">[</span>36<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-SA-20190731_37-0" class="reference"><a href="#cite_note-SA-20190731-37"><span class="cite-bracket">[</span>37<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-NA-20191113_38-0" class="reference"><a href="#cite_note-NA-20191113-38"><span class="cite-bracket">[</span>38<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-BA-20191113_39-0" class="reference"><a href="#cite_note-BA-20191113-39"><span class="cite-bracket">[</span>39<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading5"><h5 id="Origin_of_hypervelocity_stars">Origin of hypervelocity stars</h5><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=9" title="Edit section: Origin of hypervelocity 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:Runaway_star_speeding_from_30_Doradus.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/2/25/Runaway_star_speeding_from_30_Doradus.jpg/220px-Runaway_star_speeding_from_30_Doradus.jpg" decoding="async" width="220" height="176" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/2/25/Runaway_star_speeding_from_30_Doradus.jpg/330px-Runaway_star_speeding_from_30_Doradus.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/2/25/Runaway_star_speeding_from_30_Doradus.jpg/440px-Runaway_star_speeding_from_30_Doradus.jpg 2x" data-file-width="3000" data-file-height="2400" /></a><figcaption>Runaway star speeding from 30 Doradus. Image taken by the Hubble Space Telescope.</figcaption></figure> <p>HVSs are believed to predominantly originate by close encounters of <a href="/wiki/Binary_star" title="Binary star">binary stars</a> with the <a href="/wiki/Supermassive_black_hole" title="Supermassive black hole">supermassive black hole</a> in the center of the <a href="/wiki/Milky_Way" title="Milky Way">Milky Way</a>. One of the two partners is gravitationally captured by the <a href="/wiki/Black_hole" title="Black hole">black hole</a> (in the sense of entering orbit around it), while the other escapes with high velocity, becoming a HVS. Such maneuvers are analogous to the capture and ejection of <a href="/wiki/Interstellar_object" title="Interstellar object">interstellar objects</a> by a star. </p><p>Supernova-induced HVSs may also be possible, although they are presumably rare. In this scenario, a HVS is ejected from a close binary system as a result of the companion star undergoing a supernova explosion. Ejection velocities up to 770 km/s, as measured from the galactic rest frame, are possible for late-type B-stars.<sup id="cite_ref-40" class="reference"><a href="#cite_note-40"><span class="cite-bracket">[</span>40<span class="cite-bracket">]</span></a></sup> This mechanism can explain the origin of HVSs which are ejected from the galactic disk. </p><p>Known HVSs are <a href="/wiki/Main_sequence" title="Main sequence">main-sequence</a> stars with masses a few times that of the Sun. HVSs with smaller masses are also expected and G/K-dwarf HVS candidates have been found. </p><p>Some HVSs may have originated from a disrupted dwarf galaxy. When it made its closest approach to the center of the Milky Way, some of its stars broke free and were thrown into space, due to the <a href="/wiki/Gravity_assist" title="Gravity assist">slingshot-like</a> effect of the boost.<sup id="cite_ref-41" class="reference"><a href="#cite_note-41"><span class="cite-bracket">[</span>41<span class="cite-bracket">]</span></a></sup> </p><p>Some <a href="/wiki/Neutron_star" title="Neutron star">neutron stars</a> are inferred to be traveling with similar speeds. This could be related to HVSs and the HVS ejection mechanism. Neutron stars are the remnants of <a href="/wiki/Supernova" title="Supernova">supernova</a> explosions, and their extreme speeds are very likely the result of an asymmetric supernova explosion or the loss of their near partner during the supernova explosions that forms them. The neutron star <a href="/wiki/RX_J0822-4300" class="mw-redirect" title="RX J0822-4300">RX J0822-4300</a>, which was measured to move at a record speed of over 1,500 km/s (0.5% of the <a href="/wiki/Speed_of_light" title="Speed of light">speed of light</a>) in 2007 by the <a href="/wiki/Chandra_X-ray_Observatory" title="Chandra X-ray Observatory">Chandra X-ray Observatory</a>, is thought to have been produced the first way.<sup id="cite_ref-42" class="reference"><a href="#cite_note-42"><span class="cite-bracket">[</span>42<span class="cite-bracket">]</span></a></sup> </p><p>One theory regarding the ignition of Type Ia supernovae invokes the onset of a merger between two white dwarfs in a binary star system, triggering the explosion of the more massive white dwarf. If the less massive white dwarf is not destroyed during the explosion, it will no longer be gravitationally bound to its destroyed companion, causing it to leave the system as a hypervelocity star with its pre-explosion orbital velocity of 1000–2500 km/s. In 2018, three such stars were discovered using data from the Gaia satellite.<sup id="cite_ref-43" class="reference"><a href="#cite_note-43"><span class="cite-bracket">[</span>43<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading5"><h5 id="Partial_list_of_HVSs">Partial list of HVSs</h5><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=10" title="Edit section: Partial list of HVSs"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>As of 2014, twenty HVS were known.<sup id="cite_ref-44" class="reference"><a href="#cite_note-44"><span class="cite-bracket">[</span>44<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-apj671_2_1708_31-1" class="reference"><a href="#cite_note-apj671_2_1708-31"><span class="cite-bracket">[</span>31<span class="cite-bracket">]</span></a></sup> </p> <ul><li>HVS 1 – (<a href="/wiki/SDSS_J090745.0%2B024507" title="SDSS J090745.0+024507">SDSS J090744.99+024506.8</a>) (a.k.a. The Outcast Star) – the first hypervelocity star to be discovered<sup id="cite_ref-HVS1_27-1" class="reference"><a href="#cite_note-HVS1-27"><span class="cite-bracket">[</span>27<span class="cite-bracket">]</span></a></sup></li> <li>HVS 2 – (SDSS J093320.86+441705.4 <i>or</i> <a href="/wiki/US_708" title="US 708">US 708</a>)</li> <li>HVS 3 – (<a href="/wiki/HE_0437-5439" title="HE 0437-5439">HE 0437-5439</a>) – possibly from the <a href="/wiki/Large_Magellanic_Cloud" title="Large Magellanic Cloud">Large Magellanic Cloud</a><sup id="cite_ref-HVS3_28-1" class="reference"><a href="#cite_note-HVS3-28"><span class="cite-bracket">[</span>28<span class="cite-bracket">]</span></a></sup></li> <li>HVS 4 – (<a href="/w/index.php?title=SDSS_J091301.00%2B305120.0&action=edit&redlink=1" class="new" title="SDSS J091301.00+305120.0 (page does not exist)">SDSS J091301.00+305120.0</a>)</li> <li>HVS 5 – (<a href="/w/index.php?title=SDSS_J091759.42%2B672238.7&action=edit&redlink=1" class="new" title="SDSS J091759.42+672238.7 (page does not exist)">SDSS J091759.42+672238.7</a>)</li> <li>HVS 6 – (<a href="/w/index.php?title=SDSS_J110557.45%2B093439.5&action=edit&redlink=1" class="new" title="SDSS J110557.45+093439.5 (page does not exist)">SDSS J110557.45+093439.5</a>)</li> <li><a href="/wiki/HVS_7" title="HVS 7">HVS 7</a> – (SDSS J113312.12+010824.9)</li> <li>HVS 8 – (<a href="/w/index.php?title=SDSS_J094214.04%2B200322.1&action=edit&redlink=1" class="new" title="SDSS J094214.04+200322.1 (page does not exist)">SDSS J094214.04+200322.1</a>)</li> <li>HVS 9 – (<a href="/w/index.php?title=SDSS_J102137.08-005234.8&action=edit&redlink=1" class="new" title="SDSS J102137.08-005234.8 (page does not exist)">SDSS J102137.08-005234.8</a>)</li> <li>HVS 10 – (<a href="/w/index.php?title=SDSS_J120337.85%2B180250.4&action=edit&redlink=1" class="new" title="SDSS J120337.85+180250.4 (page does not exist)">SDSS J120337.85+180250.4</a>)</li></ul> <div class="mw-heading mw-heading2"><h2 id="Kinematic_groups">Kinematic groups</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=11" title="Edit section: Kinematic groups"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>A set of stars with similar space motion and ages is known as a kinematic group.<sup id="cite_ref-Santiago_45-0" class="reference"><a href="#cite_note-Santiago-45"><span class="cite-bracket">[</span>45<span class="cite-bracket">]</span></a></sup> These are stars that could share a common origin, such as the evaporation of an <a href="/wiki/Open_cluster" title="Open cluster">open cluster</a>, the remains of a star forming region, or collections of overlapping star formation bursts at differing time periods in adjacent regions.<sup id="cite_ref-mnras328_1_45_46-0" class="reference"><a href="#cite_note-mnras328_1_45-46"><span class="cite-bracket">[</span>46<span class="cite-bracket">]</span></a></sup> Most stars are born within <a href="/wiki/Molecular_cloud" title="Molecular cloud">molecular clouds</a> known as <a href="/wiki/Molecular_cloud" title="Molecular cloud">stellar nurseries</a>. The stars formed within such a cloud compose gravitationally bound <a href="/wiki/Open_clusters" class="mw-redirect" title="Open clusters">open clusters</a> containing dozens to thousands of members with similar ages and compositions. These clusters dissociate with time. Groups of young stars that escape a cluster, or are no longer bound to each other, form stellar associations. As these stars age and disperse, their association is no longer readily apparent and they become moving groups of stars. </p><p>Astronomers are able to determine if stars are members of a kinematic group because they share the same age, <a href="/wiki/Metallicity" title="Metallicity">metallicity</a>, and kinematics (<a href="/wiki/Radial_velocity" title="Radial velocity">radial velocity</a> and <a href="/wiki/Proper_motion" title="Proper motion">proper motion</a>). As the stars in a moving group formed in proximity and at nearly the same time from the same gas cloud, although later disrupted by tidal forces, they share similar characteristics.<sup id="cite_ref-47" class="reference"><a href="#cite_note-47"><span class="cite-bracket">[</span>47<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading3"><h3 id="Stellar_associations">Stellar associations</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=12" title="Edit section: Stellar associations"><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/Stellar_association" title="Stellar association">Stellar association</a></div> <p>A stellar association is a very loose <a href="/wiki/Star_cluster" title="Star cluster">star cluster</a>, whose stars share a common origin and are still moving together through space, but have become gravitationally unbound. Associations are primarily identified by their common movement vectors and ages. Identification by chemical composition is also used to factor in association memberships. </p><p>Stellar associations were first discovered by the <a href="/wiki/Armenia" title="Armenia">Armenian</a> astronomer <a href="/wiki/Viktor_Ambartsumian" title="Viktor Ambartsumian">Viktor Ambartsumian</a> in 1947.<sup id="cite_ref-baas29_48-0" class="reference"><a href="#cite_note-baas29-48"><span class="cite-bracket">[</span>48<span class="cite-bracket">]</span></a></sup> The conventional name for an association uses the names or abbreviations of the <a href="/wiki/Constellation" title="Constellation">constellation</a> (or constellations) in which they are located; the association type, and, sometimes, a numerical identifier. </p> <div class="mw-heading mw-heading4"><h4 id="Types">Types</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=13" title="Edit section: Types"><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:Infrared_VISTA_view_of_a_nearby_star_formation_in_Monoceros.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/7/7f/Infrared_VISTA_view_of_a_nearby_star_formation_in_Monoceros.jpg/220px-Infrared_VISTA_view_of_a_nearby_star_formation_in_Monoceros.jpg" decoding="async" width="220" height="174" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/7/7f/Infrared_VISTA_view_of_a_nearby_star_formation_in_Monoceros.jpg/330px-Infrared_VISTA_view_of_a_nearby_star_formation_in_Monoceros.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/7/7f/Infrared_VISTA_view_of_a_nearby_star_formation_in_Monoceros.jpg/440px-Infrared_VISTA_view_of_a_nearby_star_formation_in_Monoceros.jpg 2x" data-file-width="10065" data-file-height="7942" /></a><figcaption>Infrared <a href="/wiki/ESO" class="mw-redirect" title="ESO">ESO</a>'s <a href="/wiki/VISTA_(telescope)" title="VISTA (telescope)">VISTA</a> view of a stellar nursery in <a href="/wiki/Monoceros_(constellation)" class="mw-redirect" title="Monoceros (constellation)">Monoceros</a></figcaption></figure> <p>Viktor Ambartsumian first categorized stellar associations into two groups, OB and T, based on the properties of their stars.<sup id="cite_ref-baas29_48-1" class="reference"><a href="#cite_note-baas29-48"><span class="cite-bracket">[</span>48<span class="cite-bracket">]</span></a></sup> A third category, R, was later suggested by <a href="/wiki/Sidney_van_den_Bergh" title="Sidney van den Bergh">Sidney van den Bergh</a> for associations that illuminate <a href="/wiki/Reflection_nebula" title="Reflection nebula">reflection nebulae</a>.<sup id="cite_ref-ra1_49-0" class="reference"><a href="#cite_note-ra1-49"><span class="cite-bracket">[</span>49<span class="cite-bracket">]</span></a></sup> The OB, T, and R associations form a continuum of young stellar groupings. But it is currently uncertain whether they are an evolutionary sequence, or represent some other factor at work.<sup id="cite_ref-Mon_R2_50-0" class="reference"><a href="#cite_note-Mon_R2-50"><span class="cite-bracket">[</span>50<span class="cite-bracket">]</span></a></sup> Some groups also display properties of both OB and T associations, so the categorization is not always clear-cut. </p> <div class="mw-heading mw-heading4"><h4 id="OB_associations">OB associations</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=14" title="Edit section: OB associations"><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:Carina_Nebula.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/e/ea/Carina_Nebula.jpg/220px-Carina_Nebula.jpg" decoding="async" width="220" height="150" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/e/ea/Carina_Nebula.jpg/330px-Carina_Nebula.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/e/ea/Carina_Nebula.jpg/440px-Carina_Nebula.jpg 2x" data-file-width="13092" data-file-height="8926" /></a><figcaption><a href="/wiki/Carina_OB1" title="Carina OB1">Carina OB1</a>, a large OB association</figcaption></figure> <p>Young associations will contain 10 to 100 massive stars of <a href="/wiki/Stellar_classification" title="Stellar classification">spectral class</a> <a href="/wiki/O-type_star" title="O-type star">O</a> and <a href="/wiki/Stellar_classification" title="Stellar classification">B</a>, and are known as <i>OB associations</i>. In addition, these associations also contain hundreds or thousands of low- and intermediate-mass stars. Association members are believed to form within the same small volume inside a giant <a href="/wiki/Molecular_cloud" title="Molecular cloud">molecular cloud</a>. Once the surrounding dust and gas is blown away, the remaining stars become unbound and begin to drift apart.<sup id="cite_ref-GAIA_51-0" class="reference"><a href="#cite_note-GAIA-51"><span class="cite-bracket">[</span>51<span class="cite-bracket">]</span></a></sup> It is believed that the majority of all stars in the Milky Way were formed in OB associations.<sup id="cite_ref-GAIA_51-1" class="reference"><a href="#cite_note-GAIA-51"><span class="cite-bracket">[</span>51<span class="cite-bracket">]</span></a></sup> <a href="/wiki/O-type_star" title="O-type star">O-class stars</a> are short-lived, and will expire as <a href="/wiki/Supernova" title="Supernova">supernovae</a> after roughly one million years. As a result, OB associations are generally only a few million years in age or less. The O-B stars in the association will have burned all their fuel within ten million years. (Compare this to the current age of the <a href="/wiki/Sun" title="Sun">Sun</a> at about five billion years.) </p><p>The <a href="/wiki/Hipparcos" title="Hipparcos">Hipparcos</a> satellite provided measurements that located a dozen OB associations within 650 <a href="/wiki/Parsec" title="Parsec">parsecs</a> of the Sun.<sup id="cite_ref-52" class="reference"><a href="#cite_note-52"><span class="cite-bracket">[</span>52<span class="cite-bracket">]</span></a></sup> The nearest OB association is the <a href="/wiki/Scorpius%E2%80%93Centaurus_association" title="Scorpius–Centaurus association">Scorpius–Centaurus association</a>, located about 400 <a href="/wiki/Light-year" title="Light-year">light-years</a> from the <a href="/wiki/Sun" title="Sun">Sun</a>.<sup id="cite_ref-53" class="reference"><a href="#cite_note-53"><span class="cite-bracket">[</span>53<span class="cite-bracket">]</span></a></sup> </p><p>OB associations have also been found in the <a href="/wiki/Large_Magellanic_Cloud" title="Large Magellanic Cloud">Large Magellanic Cloud</a> and the <a href="/wiki/Andromeda_Galaxy" title="Andromeda Galaxy">Andromeda Galaxy</a>. These associations can be quite sparse, spanning 1,500 light-years in diameter.<sup id="cite_ref-AS1998_17-1" class="reference"><a href="#cite_note-AS1998-17"><span class="cite-bracket">[</span>17<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading4"><h4 id="T_associations">T associations</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=15" title="Edit section: T associations"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Young stellar groups can contain a number of infant <a href="/wiki/T_Tauri_star" title="T Tauri star">T Tauri stars</a> that are still in the process of entering the <a href="/wiki/Main_sequence" title="Main sequence">main sequence</a>. These sparse populations of up to a thousand T Tauri stars are known as <i>T associations</i>. The nearest example is the <a href="/w/index.php?title=Taurus-Auriga_T_association&action=edit&redlink=1" class="new" title="Taurus-Auriga T association (page does not exist)">Taurus-Auriga T association</a> (Tau–Aur T association), located at a distance of 140 <a href="/wiki/Parsec" title="Parsec">parsecs</a> from the Sun.<sup id="cite_ref-54" class="reference"><a href="#cite_note-54"><span class="cite-bracket">[</span>54<span class="cite-bracket">]</span></a></sup> Other examples of T associations include the <a href="/w/index.php?title=R_Corona_Australis_T_association&action=edit&redlink=1" class="new" title="R Corona Australis T association (page does not exist)">R Corona Australis T association</a>, the <a href="/w/index.php?title=Lupus_T_association&action=edit&redlink=1" class="new" title="Lupus T association (page does not exist)">Lupus T association</a>, the <a href="/w/index.php?title=Chamaeleon_T_association&action=edit&redlink=1" class="new" title="Chamaeleon T association (page does not exist)">Chamaeleon T association</a> and the <a href="/w/index.php?title=Velorum_T_association&action=edit&redlink=1" class="new" title="Velorum T association (page does not exist)">Velorum T association</a>. T associations are often found in the vicinity of the molecular cloud from which they formed. Some, but not all, include O–B class stars. Group members have the same age and origin, the same chemical composition, and the same amplitude and direction in their vector of velocity. </p> <div class="mw-heading mw-heading4"><h4 id="R_associations">R associations</h4><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=16" title="Edit section: R associations"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Associations of stars that illuminate reflection <a href="/wiki/Nebula" title="Nebula">nebulae</a> are called <i>R associations</i>, a name suggested by Sidney van den Bergh after he discovered that the stars in these nebulae had a non-uniform distribution.<sup id="cite_ref-ra1_49-1" class="reference"><a href="#cite_note-ra1-49"><span class="cite-bracket">[</span>49<span class="cite-bracket">]</span></a></sup> These young stellar groupings contain main sequence stars that are not sufficiently massive to disperse the interstellar clouds in which they formed.<sup id="cite_ref-Mon_R2_50-1" class="reference"><a href="#cite_note-Mon_R2-50"><span class="cite-bracket">[</span>50<span class="cite-bracket">]</span></a></sup> This allows the properties of the surrounding dark cloud to be examined by astronomers. Because R associations are more plentiful than OB associations, they can be used to trace out the structure of the galactic spiral arms.<sup id="cite_ref-55" class="reference"><a href="#cite_note-55"><span class="cite-bracket">[</span>55<span class="cite-bracket">]</span></a></sup> An example of an R association is <a href="/w/index.php?title=Monoceros_R2&action=edit&redlink=1" class="new" title="Monoceros R2 (page does not exist)">Monoceros R2</a>, located 830 ± 50 <a href="/wiki/Parsec" title="Parsec">parsecs</a> from the Sun.<sup id="cite_ref-Mon_R2_50-2" class="reference"><a href="#cite_note-Mon_R2-50"><span class="cite-bracket">[</span>50<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading3"><h3 id="Moving_groups">Moving groups<span class="anchor" id="moving_group_anchor"></span></h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=17" title="Edit section: Moving groups"><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">Further information: <a href="/wiki/List_of_nearby_stellar_associations_and_moving_groups" title="List of nearby stellar associations and moving groups">List of nearby stellar associations and moving groups</a></div> <figure class="mw-halign-right" typeof="mw:File/Thumb"><a href="/wiki/File:Ursa_Major_%C5%81azy.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/9/98/Ursa_Major_%C5%81azy.jpg/250px-Ursa_Major_%C5%81azy.jpg" decoding="async" width="250" height="167" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/9/98/Ursa_Major_%C5%81azy.jpg/375px-Ursa_Major_%C5%81azy.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/9/98/Ursa_Major_%C5%81azy.jpg/500px-Ursa_Major_%C5%81azy.jpg 2x" data-file-width="5184" data-file-height="3456" /></a><figcaption><a href="/wiki/Ursa_Major_Moving_Group" class="mw-redirect" title="Ursa Major Moving Group">Ursa Major Moving Group</a>, the closest stellar moving group to Earth</figcaption></figure> <p>If the remnants of a stellar association drift through the Milky Way as a somewhat coherent assemblage, then they are termed a <b>moving group</b> or <b>kinematic group</b>. Moving groups can be old, such as the <a href="/wiki/HR_1614" title="HR 1614">HR 1614</a> moving group at two billion years, or young, such as the <a href="/wiki/AB_Doradus_moving_group#Age" title="AB Doradus moving group">AB Dor Moving Group</a> at only 120 million years. </p><p>Moving groups were studied intensely by <a href="/wiki/Olin_Eggen" class="mw-redirect" title="Olin Eggen">Olin Eggen</a> in the 1960s.<sup id="cite_ref-56" class="reference"><a href="#cite_note-56"><span class="cite-bracket">[</span>56<span class="cite-bracket">]</span></a></sup> A list of the nearest young moving groups has been compiled by López-Santiago <i>et al.</i><sup id="cite_ref-Santiago_45-1" class="reference"><a href="#cite_note-Santiago-45"><span class="cite-bracket">[</span>45<span class="cite-bracket">]</span></a></sup> The closest is the <a href="/wiki/Ursa_Major_Moving_Group" class="mw-redirect" title="Ursa Major Moving Group">Ursa Major Moving Group</a> which includes all of the stars in the <a href="/wiki/Big_Dipper" title="Big Dipper">Plough / Big Dipper</a> <a href="/wiki/Asterism_(astronomy)" title="Asterism (astronomy)">asterism</a> except for <a href="/wiki/Dubhe" title="Dubhe">Dubhe</a> and <a href="/wiki/Eta_Ursae_Majoris" class="mw-redirect" title="Eta Ursae Majoris">η Ursae Majoris</a>. This is sufficiently close that the <a href="/wiki/Sun" title="Sun">Sun</a> lies in its outer fringes, without being part of the group. Hence, although members are concentrated at <a href="/wiki/Declination" title="Declination">declinations</a> near 60°N, some outliers are as far away across the sky as <a href="/wiki/Triangulum_Australe" title="Triangulum Australe">Triangulum Australe</a> at 70°S. </p><p>The list of young moving groups is constantly evolving. The Banyan Σ tool<sup id="cite_ref-57" class="reference"><a href="#cite_note-57"><span class="cite-bracket">[</span>57<span class="cite-bracket">]</span></a></sup> currently lists 29 nearby young moving groups<sup id="cite_ref-59" class="reference"><a href="#cite_note-59"><span class="cite-bracket">[</span>59<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-GagnéEtal2018a_58-1" class="reference"><a href="#cite_note-GagnéEtal2018a-58"><span class="cite-bracket">[</span>58<span class="cite-bracket">]</span></a></sup> Recent additions to nearby moving groups are the <a href="/w/index.php?title=Volans-Carina&action=edit&redlink=1" class="new" title="Volans-Carina (page does not exist)">Volans-Carina</a> Association (VCA), discovered with <a href="/wiki/Gaia_(spacecraft)" title="Gaia (spacecraft)">Gaia</a>,<sup id="cite_ref-GagnéEtal2018b_60-0" class="reference"><a href="#cite_note-GagnéEtal2018b-60"><span class="cite-bracket">[</span>60<span class="cite-bracket">]</span></a></sup> and the <a href="/wiki/Argus_Association" class="mw-redirect" title="Argus Association">Argus Association</a> (ARG), confirmed with Gaia.<sup id="cite_ref-61" class="reference"><a href="#cite_note-61"><span class="cite-bracket">[</span>61<span class="cite-bracket">]</span></a></sup> Moving groups can sometimes be further subdivided in smaller distinct groups. The Great Austral Young Association (GAYA) complex was found to be subdivided into the moving groups <i>Carina</i>, <i>Columba</i>, and <a href="/wiki/Tucana-Horologium_association" title="Tucana-Horologium association"><i>Tucana-Horologium</i></a>. The three Associations are not very distinct from each other, and have similar kinematic properties.<sup id="cite_ref-62" class="reference"><a href="#cite_note-62"><span class="cite-bracket">[</span>62<span class="cite-bracket">]</span></a></sup> </p><p>Young moving groups have well known ages and can help with the characterization of objects with hard-to-estimate <a href="/wiki/Stellar_age_estimation" title="Stellar age estimation">ages</a>, such as <a href="/wiki/Brown_dwarf#Teide_1_–_the_first_class_"M"_brown_dwarf" title="Brown dwarf">brown dwarfs</a>.<sup id="cite_ref-63" class="reference"><a href="#cite_note-63"><span class="cite-bracket">[</span>63<span class="cite-bracket">]</span></a></sup> Members of nearby young moving groups are also candidates for directly imaged <a href="/wiki/Protoplanetary_disk" title="Protoplanetary disk">protoplanetary disks</a>, such as <a href="/wiki/TW_Hydrae" title="TW Hydrae">TW Hydrae</a> or directly imaged <a href="/wiki/Exoplanet" title="Exoplanet">exoplanets</a>, such as <a href="/wiki/Beta_Pictoris_b" title="Beta Pictoris b">Beta Pictoris b</a> or <a href="/wiki/GU_Piscium_b" title="GU Piscium b">GU Psc b</a>. </p> <div class="mw-heading mw-heading3"><h3 id="Stellar_streams">Stellar streams</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=18" title="Edit section: Stellar streams"><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/List_of_stellar_streams" title="List of stellar streams">List of stellar streams</a></div> <p>A <b>stellar stream</b> is an association of <a href="/wiki/Star" title="Star">stars</a> orbiting a <a href="/wiki/Galaxy" title="Galaxy">galaxy</a> that was once a <a href="/wiki/Globular_cluster" title="Globular cluster">globular cluster</a> or <a href="/wiki/Dwarf_galaxy" title="Dwarf galaxy">dwarf galaxy</a> that has now been torn apart and stretched out along its orbit by tidal forces.<sup id="cite_ref-64" class="reference"><a href="#cite_note-64"><span class="cite-bracket">[</span>64<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading3"><h3 id="Known_kinematic_groups">Known kinematic groups</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=19" title="Edit section: Known kinematic groups"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Some nearby kinematic groups include:<sup id="cite_ref-Santiago_45-2" class="reference"><a href="#cite_note-Santiago-45"><span class="cite-bracket">[</span>45<span class="cite-bracket">]</span></a></sup> </p> <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" style="column-width: 27em;"> <ul><li>Local Association (<a href="/wiki/Pleiades" title="Pleiades">Pleiades</a> moving group)</li> <li><a href="/wiki/AB_Doradus_moving_group" title="AB Doradus moving group">AB Doradus moving group</a></li> <li><a href="/wiki/Alpha_Persei_moving_cluster" class="mw-redirect" title="Alpha Persei moving cluster">Alpha Persei moving cluster</a></li> <li><a href="/wiki/Beta_Pictoris_moving_group" title="Beta Pictoris moving group">Beta Pictoris moving group</a><sup id="cite_ref-Song2003_65-0" class="reference"><a href="#cite_note-Song2003-65"><span class="cite-bracket">[</span>65<span class="cite-bracket">]</span></a></sup></li> <li><a href="/wiki/Castor_Moving_Group" title="Castor Moving Group">Castor moving group</a></li> <li><a href="/wiki/Corona_Australis_association" class="mw-redirect" title="Corona Australis association">Corona Australis association</a></li> <li><a href="/wiki/Eta_Chamaeleontis_cluster" class="mw-redirect" title="Eta Chamaeleontis cluster">Eta Chamaeleontis cluster</a></li> <li>Hercules-Lyra association<sup id="cite_ref-Santiago_45-3" class="reference"><a href="#cite_note-Santiago-45"><span class="cite-bracket">[</span>45<span class="cite-bracket">]</span></a></sup></li> <li><a href="/wiki/Hercules_stream" title="Hercules stream">Hercules stream</a></li> <li><a href="/wiki/Hyades_Stream" title="Hyades Stream">Hyades Stream</a></li> <li><a href="/wiki/IC_2391" title="IC 2391">IC 2391</a> supercluster (Argus Association)</li> <li><a href="/w/index.php?title=Kapteyn_group&action=edit&redlink=1" class="new" title="Kapteyn group (page does not exist)">Kapteyn group</a><sup id="cite_ref-Wylie-de_Boer_2010_66-0" class="reference"><a href="#cite_note-Wylie-de_Boer_2010-66"><span class="cite-bracket">[</span>66<span class="cite-bracket">]</span></a></sup></li> <li><a href="/w/index.php?title=MBM_12_association&action=edit&redlink=1" class="new" title="MBM 12 association (page does not exist)">MBM 12 association</a></li> <li><a href="/wiki/TW_Hydrae_association" title="TW Hydrae association">TW Hydrae association</a><sup id="cite_ref-Song2003_65-1" class="reference"><a href="#cite_note-Song2003-65"><span class="cite-bracket">[</span>65<span class="cite-bracket">]</span></a></sup></li> <li><a href="/wiki/Ursa_Major_Moving_Group" class="mw-redirect" title="Ursa Major Moving Group">Ursa Major Moving Group</a></li> <li><a href="/wiki/Wolf_630_moving_group" class="mw-redirect" title="Wolf 630 moving group">Wolf 630 moving group</a><sup id="cite_ref-McDonald1983_67-0" class="reference"><a href="#cite_note-McDonald1983-67"><span class="cite-bracket">[</span>67<span class="cite-bracket">]</span></a></sup></li> <li><a href="/wiki/Zeta_Herculis_moving_group" class="mw-redirect" title="Zeta Herculis moving group">Zeta Herculis moving group</a></li> <li><a href="/wiki/Pisces-Eridanus_stellar_stream" class="mw-redirect" title="Pisces-Eridanus stellar stream">Pisces-Eridanus stellar stream</a></li> <li><a href="/wiki/Tucana-Horologium_association" title="Tucana-Horologium association">Tucana-Horologium association</a><sup id="cite_ref-Song2003_65-2" class="reference"><a href="#cite_note-Song2003-65"><span class="cite-bracket">[</span>65<span class="cite-bracket">]</span></a></sup></li></ul></div> <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=Stellar_kinematics&action=edit&section=20" title="Edit section: See also"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <ul><li><a href="/wiki/Astrometry" title="Astrometry">Astrometry</a></li> <li><a href="/wiki/Gaia_(spacecraft)" title="Gaia (spacecraft)"><i>Gaia</i> (spacecraft)</a></li> <li><a href="/wiki/Hipparcos" title="Hipparcos">Hipparcos</a></li> <li><a href="/wiki/N-body_problem" title="N-body problem">n-body problem</a></li> <li><a href="/wiki/Open_cluster_remnant" title="Open cluster remnant">Open cluster remnant</a></li> <li><a href="/wiki/List_of_nearby_stellar_associations_and_moving_groups" title="List of nearby stellar associations and moving groups">List of nearby stellar associations and moving groups</a></li> <li><a href="/wiki/Stellar_association" title="Stellar association">Stellar association</a></li></ul> <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=Stellar_kinematics&action=edit&section=21" title="Edit section: References"><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 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Retrieved <span class="nowrap">2019-11-15</span></span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=unknown&rft.jtitle=www.exoplanetes.umontreal.ca&rft.atitle=BANYAN+%CE%A3&rft_id=http%3A%2F%2Fwww.exoplanetes.umontreal.ca%2Fbanyan%2Fbanyansigma.php&rfr_id=info%3Asid%2Fen.wikipedia.org%3AStellar+kinematics" class="Z3988"></span></span> </li> <li id="cite_note-GagnéEtal2018a-58"><span class="mw-cite-backlink">^ <a href="#cite_ref-GagnéEtal2018a_58-0"><sup><i><b>a</b></i></sup></a> <a href="#cite_ref-GagnéEtal2018a_58-1"><sup><i><b>b</b></i></sup></a></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFGagnéMamajekMaloRiedel2018" class="citation journal cs1">Gagné, Jonathan; Mamajek, Eric E.; Malo, Lison; Riedel, Adric; Rodriguez, David; Lafrenière, David; et al. (2018-03-21). <a rel="nofollow" class="external text" href="https://doi.org/10.3847%2F1538-4357%2Faaae09">"The BANYAN Σ multivariate Bayesian algorithm to identify members of young associations with 150 pc"</a>. <i>The Astrophysical Journal</i>. BANYAN XI. <b>856</b> (1): 23. <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/1801.09051">1801.09051</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/2018ApJ...856...23G">2018ApJ...856...23G</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<span class="id-lock-free" title="Freely accessible"><a rel="nofollow" class="external text" href="https://doi.org/10.3847%2F1538-4357%2Faaae09">10.3847/1538-4357/aaae09</a></span>. <a href="/wiki/ISSN_(identifier)" class="mw-redirect" title="ISSN (identifier)">ISSN</a> <a rel="nofollow" class="external text" href="https://search.worldcat.org/issn/0004-637X">0004-637X</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:119185386">119185386</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=The+BANYAN+%CE%A3+multivariate+Bayesian+algorithm+to+identify+members+of+young+associations+with+150+pc&rft.volume=856&rft.issue=1&rft.pages=23&rft.date=2018-03-21&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A119185386%23id-name%3DS2CID&rft_id=info%3Abibcode%2F2018ApJ...856...23G&rft_id=info%3Aarxiv%2F1801.09051&rft.issn=0004-637X&rft_id=info%3Adoi%2F10.3847%2F1538-4357%2Faaae09&rft.aulast=Gagn%C3%A9&rft.aufirst=Jonathan&rft.au=Mamajek%2C+Eric+E.&rft.au=Malo%2C+Lison&rft.au=Riedel%2C+Adric&rft.au=Rodriguez%2C+David&rft.au=Lafreni%C3%A8re%2C+David&rft.au=Faherty%2C+Jacqueline+K.&rft.au=Roy-Loubier%2C+Olivier&rft.au=Pueyo%2C+Laurent&rft.au=Robin%2C+Annie+C.&rft.au=Doyon%2C+Ren%C3%A9&rft_id=https%3A%2F%2Fdoi.org%2F10.3847%252F1538-4357%252Faaae09&rfr_id=info%3Asid%2Fen.wikipedia.org%3AStellar+kinematics" class="Z3988"></span></span> </li> <li id="cite_note-59"><span class="mw-cite-backlink"><b><a href="#cite_ref-59">^</a></b></span> <span class="reference-text">See <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFGagnéMamajekMaloRiedel2018" class="citation journal cs1">Gagné, Jonathan; Mamajek, Eric E.; Malo, Lison; Riedel, Adric; Rodriguez, David; Lafrenière, David; <a href="/wiki/Jackie_Faherty" title="Jackie Faherty">Faherty, Jacqueline K.</a>; Roy-Loubier, Olivier; Pueyo, Laurent; Robin, Annie C.; Doyon, René (2018). <a rel="nofollow" class="external text" href="https://doi.org/10.3847%2F1538-4357%2Faaae09">"Figures 4 & 5 of Gagné <i>et al</i>. 2018a"</a>. <i>The Astrophysical Journal</i>. <b>856</b> (1): 23. <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/1801.09051">1801.09051</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/2018ApJ...856...23G">2018ApJ...856...23G</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<span class="id-lock-free" title="Freely accessible"><a rel="nofollow" class="external text" href="https://doi.org/10.3847%2F1538-4357%2Faaae09">10.3847/1538-4357/aaae09</a></span>. <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:119185386">119185386</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=Figures+4+%26+5+of+Gagn%C3%A9+et+al.+2018a&rft.volume=856&rft.issue=1&rft.pages=23&rft.date=2018&rft_id=info%3Aarxiv%2F1801.09051&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A119185386%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.3847%2F1538-4357%2Faaae09&rft_id=info%3Abibcode%2F2018ApJ...856...23G&rft.aulast=Gagn%C3%A9&rft.aufirst=Jonathan&rft.au=Mamajek%2C+Eric+E.&rft.au=Malo%2C+Lison&rft.au=Riedel%2C+Adric&rft.au=Rodriguez%2C+David&rft.au=Lafreni%C3%A8re%2C+David&rft.au=Faherty%2C+Jacqueline+K.&rft.au=Roy-Loubier%2C+Olivier&rft.au=Pueyo%2C+Laurent&rft.au=Robin%2C+Annie+C.&rft.au=Doyon%2C+Ren%C3%A9&rft_id=https%3A%2F%2Fdoi.org%2F10.3847%252F1538-4357%252Faaae09&rfr_id=info%3Asid%2Fen.wikipedia.org%3AStellar+kinematics" class="Z3988"></span><sup id="cite_ref-GagnéEtal2018a_58-0" class="reference"><a href="#cite_note-GagnéEtal2018a-58"><span class="cite-bracket">[</span>58<span class="cite-bracket">]</span></a></sup></span> </li> <li id="cite_note-GagnéEtal2018b-60"><span class="mw-cite-backlink"><b><a href="#cite_ref-GagnéEtal2018b_60-0">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFGagnéFahertyMamajek2018" class="citation journal cs1">Gagné, Jonathan; 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"A near-infrared spectroscopic study of young field ultra-cool dwarfs". <i>The Astrophysical Journal</i>. <b>772</b> (2): 79. <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/1305.4418">1305.4418</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/2013ApJ...772...79A">2013ApJ...772...79A</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1088%2F0004-637X%2F772%2F2%2F79">10.1088/0004-637X/772/2/79</a>. <a href="/wiki/ISSN_(identifier)" class="mw-redirect" title="ISSN (identifier)">ISSN</a> <a rel="nofollow" class="external text" href="https://search.worldcat.org/issn/0004-637X">0004-637X</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:59289573">59289573</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=A+near-infrared+spectroscopic+study+of+young+field+ultra-cool+dwarfs&rft.volume=772&rft.issue=2&rft.pages=79&rft.date=2013-07-09&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A59289573%23id-name%3DS2CID&rft_id=info%3Abibcode%2F2013ApJ...772...79A&rft_id=info%3Aarxiv%2F1305.4418&rft.issn=0004-637X&rft_id=info%3Adoi%2F10.1088%2F0004-637X%2F772%2F2%2F79&rft.aulast=Allers&rft.aufirst=K.N.&rft.au=Liu%2C+Michael+C.&rfr_id=info%3Asid%2Fen.wikipedia.org%3AStellar+kinematics" class="Z3988"></span></span> </li> <li id="cite_note-64"><span class="mw-cite-backlink"><b><a href="#cite_ref-64">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFSchilling2022" class="citation web cs1">Schilling, Govert (January 12, 2022). <a rel="nofollow" class="external text" href="https://skyandtelescope.org/astronomy-news/stellar-streams-are-revealing-their-secrets/">"Stellar streams are revealing their secrets"</a>. Sky & Telescope<span class="reference-accessdate">. Retrieved <span class="nowrap">December 13,</span> 2022</span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=Stellar+streams+are+revealing+their+secrets&rft.pub=Sky+%26+Telescope&rft.date=2022-01-12&rft.aulast=Schilling&rft.aufirst=Govert&rft_id=https%3A%2F%2Fskyandtelescope.org%2Fastronomy-news%2Fstellar-streams-are-revealing-their-secrets%2F&rfr_id=info%3Asid%2Fen.wikipedia.org%3AStellar+kinematics" class="Z3988"></span></span> </li> <li id="cite_note-Song2003-65"><span class="mw-cite-backlink">^ <a href="#cite_ref-Song2003_65-0"><sup><i><b>a</b></i></sup></a> <a href="#cite_ref-Song2003_65-1"><sup><i><b>b</b></i></sup></a> <a href="#cite_ref-Song2003_65-2"><sup><i><b>c</b></i></sup></a></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFSongZuckermanBessell2003" class="citation journal cs1">Song, Inseok; et al. (December 2003). <a rel="nofollow" class="external text" href="http://astro.berkeley.edu/~kalas/disksite/library/song03.pdf">"New Members of the TW Hydrae Association, β Pictoris Moving Group, and Tucana/Horologium Association"</a> <span class="cs1-format">(PDF)</span>. <i>The Astrophysical Journal</i>. <b>599</b> (1): 342–350. <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...599..342S">2003ApJ...599..342S</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%2F379194">10.1086/379194</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:51833191">51833191</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=New+Members+of+the+TW+Hydrae+Association%2C+%CE%B2+Pictoris+Moving+Group%2C+and+Tucana%2FHorologium+Association&rft.volume=599&rft.issue=1&rft.pages=342-350&rft.date=2003-12&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A51833191%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.1086%2F379194&rft_id=info%3Abibcode%2F2003ApJ...599..342S&rft.aulast=Song&rft.aufirst=Inseok&rft.au=Zuckerman%2C+B.&rft.au=Bessell%2C+M.+S.&rft_id=http%3A%2F%2Fastro.berkeley.edu%2F~kalas%2Fdisksite%2Flibrary%2Fsong03.pdf&rfr_id=info%3Asid%2Fen.wikipedia.org%3AStellar+kinematics" class="Z3988"></span></span> </li> <li id="cite_note-Wylie-de_Boer_2010-66"><span class="mw-cite-backlink"><b><a href="#cite_ref-Wylie-de_Boer_2010_66-0">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFWylie-de_BoerFreemanWilliams2010" class="citation journal cs1">Wylie-de Boer, Elizabeth; et al. (February 2010). "Evidence of Tidal Debris from ω Cen in the Kapteyn Group". <i>The Astronomical Journal</i>. <b>139</b> (2): 636–645. <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/0910.3735">0910.3735</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/2010AJ....139..636W">2010AJ....139..636W</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1088%2F0004-6256%2F139%2F2%2F636">10.1088/0004-6256/139/2/636</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:119217292">119217292</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=The+Astronomical+Journal&rft.atitle=Evidence+of+Tidal+Debris+from+%CF%89+Cen+in+the+Kapteyn+Group&rft.volume=139&rft.issue=2&rft.pages=636-645&rft.date=2010-02&rft_id=info%3Aarxiv%2F0910.3735&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A119217292%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.1088%2F0004-6256%2F139%2F2%2F636&rft_id=info%3Abibcode%2F2010AJ....139..636W&rft.aulast=Wylie-de+Boer&rft.aufirst=Elizabeth&rft.au=Freeman%2C+Ken&rft.au=Williams%2C+Mary&rfr_id=info%3Asid%2Fen.wikipedia.org%3AStellar+kinematics" class="Z3988"></span></span> </li> <li id="cite_note-McDonald1983-67"><span class="mw-cite-backlink"><b><a href="#cite_ref-McDonald1983_67-0">^</a></b></span> <span class="reference-text"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFMcDonaldHearnshaw1983" class="citation journal cs1">McDonald, A. R. E.; Hearnshaw, J. B. (August 1983). <a rel="nofollow" class="external text" href="https://doi.org/10.1093%2Fmnras%2F204.3.841">"The Wolf 630 moving group of stars"</a>. <i>Monthly Notices of the Royal Astronomical Society</i>. <b>204</b> (3): 841–852. <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/1983MNRAS.204..841M">1983MNRAS.204..841M</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<span class="id-lock-free" title="Freely accessible"><a rel="nofollow" class="external text" href="https://doi.org/10.1093%2Fmnras%2F204.3.841">10.1093/mnras/204.3.841</a></span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Monthly+Notices+of+the+Royal+Astronomical+Society&rft.atitle=The+Wolf+630+moving+group+of+stars&rft.volume=204&rft.issue=3&rft.pages=841-852&rft.date=1983-08&rft_id=info%3Adoi%2F10.1093%2Fmnras%2F204.3.841&rft_id=info%3Abibcode%2F1983MNRAS.204..841M&rft.aulast=McDonald&rft.aufirst=A.+R.+E.&rft.au=Hearnshaw%2C+J.+B.&rft_id=https%3A%2F%2Fdoi.org%2F10.1093%252Fmnras%252F204.3.841&rfr_id=info%3Asid%2Fen.wikipedia.org%3AStellar+kinematics" class="Z3988"></span></span> </li> </ol></div> <div class="mw-heading mw-heading2"><h2 id="Further_reading">Further reading</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Stellar_kinematics&action=edit&section=22" title="Edit section: Further reading"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <ul><li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFMajewski2006" class="citation web cs1">Majewski, Steven R. (2006). <a rel="nofollow" class="external text" href="https://archive.today/20120125061201/http://www.astro.virginia.edu/class/majewski/astr551/lectures/VELOCITIES/velocities.html">"Stellar Motions"</a>. University of Virginia. Archived from <a rel="nofollow" class="external text" href="http://www.astro.virginia.edu/class/majewski/astr551/lectures/VELOCITIES/velocities.html">the original</a> on 2012-01-25<span class="reference-accessdate">. Retrieved <span class="nowrap">2008-02-25</span></span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=Stellar+Motions&rft.pub=University+of+Virginia&rft.date=2006&rft.aulast=Majewski&rft.aufirst=Steven+R.&rft_id=http%3A%2F%2Fwww.astro.virginia.edu%2Fclass%2Fmajewski%2Fastr551%2Flectures%2FVELOCITIES%2Fvelocities.html&rfr_id=info%3Asid%2Fen.wikipedia.org%3AStellar+kinematics" class="Z3988"></span></li> <li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite class="citation web cs1"><a rel="nofollow" class="external text" href="https://web.archive.org/web/20080216225625/http://csep10.phys.utk.edu/astr162/lect/motion/space.html">"The Space Velocity and its Components"</a>. University of Tennessee. Archived from <a rel="nofollow" class="external text" href="http://csep10.phys.utk.edu/astr162/lect/motion/space.html">the original</a> on 2008-02-16<span class="reference-accessdate">. Retrieved <span class="nowrap">2008-02-25</span></span>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=The+Space+Velocity+and+its+Components&rft.pub=University+of+Tennessee&rft_id=http%3A%2F%2Fcsep10.phys.utk.edu%2Fastr162%2Flect%2Fmotion%2Fspace.html&rfr_id=info%3Asid%2Fen.wikipedia.org%3AStellar+kinematics" class="Z3988"></span></li> <li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFBlaauw_A.Morgan_W.W.1954" class="citation journal cs1">Blaauw A.; Morgan W.W. (1954). <a rel="nofollow" class="external text" href="https://doi.org/10.1086%2F145866">"The Space Motions of AE Aurigae and mu Columbae with Respect to the Orion Nebula"</a>. <i>The Astrophysical Journal</i>. <b>119</b>: 625. <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/1954ApJ...119..625B">1954ApJ...119..625B</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<span class="id-lock-free" title="Freely accessible"><a rel="nofollow" class="external text" href="https://doi.org/10.1086%2F145866">10.1086/145866</a></span>.</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=The+Space+Motions+of+AE+Aurigae+and+mu+Columbae+with+Respect+to+the+Orion+Nebula&rft.volume=119&rft.pages=625&rft.date=1954&rft_id=info%3Adoi%2F10.1086%2F145866&rft_id=info%3Abibcode%2F1954ApJ...119..625B&rft.au=Blaauw+A.&rft.au=Morgan+W.W.&rft_id=https%3A%2F%2Fdoi.org%2F10.1086%252F145866&rfr_id=info%3Asid%2Fen.wikipedia.org%3AStellar+kinematics" class="Z3988"></span></li> <li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFHoogerwerfde_Bruijnede_Zeeuw2000" class="citation journal cs1">Hoogerwerf, R.; de Bruijne, J.H.J.; de Zeeuw, P.T. (2000). "The Origin of Runaway Stars". <i>The Astrophysical Journal</i>. <b>544</b> (2): L133. <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/0007436">astro-ph/0007436</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/2000ApJ...544L.133H">2000ApJ...544L.133H</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%2F317315">10.1086/317315</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:6725343">6725343</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=The+Origin+of+Runaway+Stars&rft.volume=544&rft.issue=2&rft.pages=L133&rft.date=2000&rft_id=info%3Aarxiv%2Fastro-ph%2F0007436&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A6725343%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.1086%2F317315&rft_id=info%3Abibcode%2F2000ApJ...544L.133H&rft.aulast=Hoogerwerf&rft.aufirst=R.&rft.au=de+Bruijne%2C+J.H.J.&rft.au=de+Zeeuw%2C+P.T.&rfr_id=info%3Asid%2Fen.wikipedia.org%3AStellar+kinematics" class="Z3988"></span></li> <li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFBrownGellerKenyonKurtz2006" class="citation journal cs1">Brown; Geller; Kenyon; Kurtz (2006). "A Successful Targeted Search for Hypervelocity Stars". <i>The Astrophysical Journal</i>. <b>640</b> (1): L35–L38. <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/0601580">astro-ph/0601580</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/2006ApJ...640L..35B">2006ApJ...640L..35B</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%2F503279">10.1086/503279</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:17220212">17220212</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=A+Successful+Targeted+Search+for+Hypervelocity+Stars&rft.volume=640&rft.issue=1&rft.pages=L35-L38&rft.date=2006&rft_id=info%3Aarxiv%2Fastro-ph%2F0601580&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A17220212%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.1086%2F503279&rft_id=info%3Abibcode%2F2006ApJ...640L..35B&rft.au=Brown&rft.au=Geller&rft.au=Kenyon&rft.au=Kurtz&rfr_id=info%3Asid%2Fen.wikipedia.org%3AStellar+kinematics" class="Z3988"></span></li> <li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFEdelmannNapiwotzkiHeberChristlieb2005" class="citation journal cs1">Edelmann, H.; Napiwotzki, R.; Heber, U.; Christlieb, N.; et al. (2005). "HE 0437-5439: An Unbound Hypervelocity Main-Sequence B-Type Star". <i>The Astrophysical Journal</i>. <b>634</b> (2): L181–L184. <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/0511321">astro-ph/0511321</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/2005ApJ...634L.181E">2005ApJ...634L.181E</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%2F498940">10.1086/498940</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:15189914">15189914</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=HE+0437-5439%3A+An+Unbound+Hypervelocity+Main-Sequence+B-Type+Star&rft.volume=634&rft.issue=2&rft.pages=L181-L184&rft.date=2005&rft_id=info%3Aarxiv%2Fastro-ph%2F0511321&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A15189914%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.1086%2F498940&rft_id=info%3Abibcode%2F2005ApJ...634L.181E&rft.aulast=Edelmann&rft.aufirst=H.&rft.au=Napiwotzki%2C+R.&rft.au=Heber%2C+U.&rft.au=Christlieb%2C+N.&rft.au=Reimers%2C+D.&rfr_id=info%3Asid%2Fen.wikipedia.org%3AStellar+kinematics" class="Z3988"></span></li></ul> <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=Stellar_kinematics&action=edit&section=23" title="Edit section: External links"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <ul><li><a rel="nofollow" class="external text" href="http://www.eso.org/outreach/press-rel/pr-1997/pr-01-97.html">ESO press release about runaway stars</a> <a rel="nofollow" class="external text" href="https://web.archive.org/web/20080516062823/http://www.eso.org/outreach/press-rel/pr-1997/pr-01-97.html">Archived</a> 2008-05-16 at the <a href="/wiki/Wayback_Machine" title="Wayback Machine">Wayback Machine</a></li> <li><a rel="nofollow" class="external text" href="http://www.daviddarling.info/encyclopedia/R/runawaystar.html">Entry in the Encyclopedia of Astrobiology, Astronomy, and Spaceflight</a></li> <li><a rel="nofollow" class="external text" href="http://www.redorbit.com/news/space/371654/two_exiled_stars_are_leaving_our_galaxy_forever/">Two Exiled Stars Are Leaving Our Galaxy Forever</a></li> <li><a rel="nofollow" class="external text" href="http://www.daviddarling.info/encyclopedia/H/hypervelocity_star.html">Entry in the Encyclopedia of Astrobiology, Astronomy, and Spaceflight</a></li> <li><a rel="nofollow" class="external free" href="https://myspaceastronomy.com/magnetar-the-most-magnetic-stars-in-the-universe-my-space/">https://myspaceastronomy.com/magnetar-the-most-magnetic-stars-in-the-universe-my-space/</a> <a rel="nofollow" class="external text" href="https://web.archive.org/web/20230306064031/https://myspaceastronomy.com/magnetar-the-most-magnetic-stars-in-the-universe-my-space/">Archived</a> 2023-03-06 at the <a href="/wiki/Wayback_Machine" title="Wayback Machine">Wayback Machine</a></li> <li><a rel="nofollow" class="external text" href="https://www.researchgate.net/publication/1779771_Young_stellar_kinematic_groups_and_their_relation_with_young_open_clusters_star_forming_regions_and_the_Gould_Belt">Young stellar kinematic groups</a>, David Montes, Departamento de Astrofísica, Universidad Complutense de Madrid.</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:" · ";font-weight:bold}.mw-parser-output .hlist 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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-Rayet_nebula" class="mw-redirect" 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 href="/wiki/Neutron_star" title="Neutron star">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" 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/Fusor_(astronomy)" title="Fusor (astronomy)">Fusor</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 class="mw-selflink selflink">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="Stellar_systems" 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" 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navbox-list navbox-odd hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Galaxy" title="Galaxy">Galaxy</a></li> <li><a href="/wiki/Dwarf_galaxy" title="Dwarf galaxy">Dwarf galaxy</a></li> <li><a href="/wiki/Star_cluster" title="Star cluster">Star cluster</a> <ul><li><a href="/wiki/Hypercompact_stellar_system" title="Hypercompact stellar system">Hypercompact stellar system</a></li> <li><a href="/wiki/Globular_cluster" title="Globular cluster">Globular cluster</a></li> <li><a href="/wiki/Dark_globular_cluster" title="Dark globular cluster">Dark globular cluster</a></li> <li><a href="/wiki/Open_cluster" title="Open cluster">Open cluster</a></li> <li><a href="/wiki/List_of_most_massive_star_clusters" title="List of most massive star clusters">List of most massive star clusters</a></li> <li><a href="/wiki/List_of_largest_star_clusters" title="List of largest star clusters">List of largest star clusters</a></li></ul></li> <li><a href="/wiki/Hypercompact_stellar_system" title="Hypercompact stellar system">Hypercompact stellar system</a></li> <li><a href="/wiki/Star_system" title="Star system">Star system</a></li> <li><a href="/wiki/Binary_star" title="Binary star">Binary star</a></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%">Unbound</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/Stellar_stream" class="mw-redirect" title="Stellar stream">Stellar stream</a></li> <li><a href="/wiki/Stellar_association" title="Stellar association">Stellar association</a></li> <li><a class="mw-selflink selflink">Moving group</a></li> <li><a href="/wiki/Runaway_star" class="mw-redirect" title="Runaway star">Runaway star</a></li> <li><a class="mw-selflink-fragment" href="#Hypervelocity_stars">Hypervelocity star</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Visual grouping</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/Double_star" title="Double star">Double star</a></li> <li><a href="/wiki/Multiple_star" class="mw-redirect" title="Multiple star">Multiple star</a></li> <li><a href="/wiki/Star_cloud" class="mw-redirect" title="Star cloud">Star cloud</a></li> <li><a href="/wiki/Asterism_(astronomy)" title="Asterism (astronomy)">Asterism</a></li> <li><a href="/wiki/Constellation" title="Constellation">Constellation</a></li></ul> </div></td></tr><tr><td class="navbox-abovebelow hlist" 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" 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