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id="toc-Cloud_collapse-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Protostar" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#Protostar"> <div class="vector-toc-text"> <span class="vector-toc-numb">3</span> <span>Protostar</span> </div> </a> <ul id="toc-Protostar-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Observations" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#Observations"> <div class="vector-toc-text"> <span class="vector-toc-numb">4</span> <span>Observations</span> </div> </a> <button aria-controls="toc-Observations-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 Observations subsection</span> </button> <ul id="toc-Observations-sublist" class="vector-toc-list"> <li id="toc-Notable_pathfinder_objects" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#Notable_pathfinder_objects"> <div class="vector-toc-text"> <span class="vector-toc-numb">4.1</span> <span>Notable pathfinder objects</span> </div> </a> <ul id="toc-Notable_pathfinder_objects-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Low_mass_and_high_mass_star_formation" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#Low_mass_and_high_mass_star_formation"> <div class="vector-toc-text"> <span class="vector-toc-numb">5</span> <span>Low mass and high mass star formation</span> </div> </a> <ul id="toc-Low_mass_and_high_mass_star_formation-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Filamentary_nature_of_star_formation" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#Filamentary_nature_of_star_formation"> <div class="vector-toc-text"> <span class="vector-toc-numb">6</span> <span>Filamentary nature of star formation</span> </div> </a> <ul id="toc-Filamentary_nature_of_star_formation-sublist" class="vector-toc-list"> </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">7</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">8</span> <span>References</span> </div> </a> <ul id="toc-References-sublist" class="vector-toc-list"> </ul> </li> </ul> </div> </div> </nav> </div> </div> <div class="mw-content-container"> <main id="content" class="mw-body"> <header class="mw-body-header vector-page-titlebar"> <nav aria-label="Contents" class="vector-toc-landmark"> <div id="vector-page-titlebar-toc" class="vector-dropdown vector-page-titlebar-toc vector-button-flush-left" > <input type="checkbox" id="vector-page-titlebar-toc-checkbox" role="button" aria-haspopup="true" data-event-name="ui.dropdown-vector-page-titlebar-toc" class="vector-dropdown-checkbox " aria-label="Toggle the table of contents" > <label id="vector-page-titlebar-toc-label" for="vector-page-titlebar-toc-checkbox" class="vector-dropdown-label cdx-button cdx-button--fake-button cdx-button--fake-button--enabled cdx-button--weight-quiet cdx-button--icon-only " aria-hidden="true" ><span class="vector-icon mw-ui-icon-listBullet mw-ui-icon-wikimedia-listBullet"></span> <span class="vector-dropdown-label-text">Toggle the table of contents</span> </label> <div class="vector-dropdown-content"> <div id="vector-page-titlebar-toc-unpinned-container" class="vector-unpinned-container"> </div> </div> </div> </nav> <h1 id="firstHeading" class="firstHeading mw-first-heading"><span class="mw-page-title-main">Star formation</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 53 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-53" 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">53 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/Stervorming" title="Stervorming – Afrikaans" lang="af" hreflang="af" data-title="Stervorming" 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%AA%D9%83%D9%88%D9%86_%D8%A7%D9%84%D9%86%D8%AC%D9%88%D9%85" title="تكون النجوم – Arabic" lang="ar" hreflang="ar" data-title="تكون النجوم" data-language-autonym="العربية" data-language-local-name="Arabic" class="interlanguage-link-target"><span>العربية</span></a></li><li class="interlanguage-link interwiki-ast mw-list-item"><a href="https://ast.wikipedia.org/wiki/Formaci%C3%B3n_estelar" title="Formación estelar – Asturian" lang="ast" hreflang="ast" data-title="Formación estelar" data-language-autonym="Asturianu" data-language-local-name="Asturian" class="interlanguage-link-target"><span>Asturianu</span></a></li><li class="interlanguage-link interwiki-bn mw-list-item"><a href="https://bn.wikipedia.org/wiki/%E0%A6%A4%E0%A6%BE%E0%A6%B0%E0%A6%BE_%E0%A6%97%E0%A6%A0%E0%A6%A8" title="তারা গঠন – Bangla" lang="bn" hreflang="bn" data-title="তারা গঠন" data-language-autonym="বাংলা" data-language-local-name="Bangla" class="interlanguage-link-target"><span>বাংলা</span></a></li><li class="interlanguage-link interwiki-bg mw-list-item"><a href="https://bg.wikipedia.org/wiki/%D0%97%D0%B2%D0%B5%D0%B7%D0%B4%D0%BE%D0%BE%D0%B1%D1%80%D0%B0%D0%B7%D1%83%D0%B2%D0%B0%D0%BD%D0%B5" title="Звездообразуване – Bulgarian" lang="bg" hreflang="bg" data-title="Звездообразуване" data-language-autonym="Български" data-language-local-name="Bulgarian" class="interlanguage-link-target"><span>Български</span></a></li><li class="interlanguage-link interwiki-bs mw-list-item"><a href="https://bs.wikipedia.org/wiki/Formiranje_zvijezda" title="Formiranje zvijezda – Bosnian" lang="bs" hreflang="bs" data-title="Formiranje zvijezda" data-language-autonym="Bosanski" data-language-local-name="Bosnian" class="interlanguage-link-target"><span>Bosanski</span></a></li><li class="interlanguage-link interwiki-ca mw-list-item"><a href="https://ca.wikipedia.org/wiki/Formaci%C3%B3_estel%C2%B7lar" title="Formació estel·lar – Catalan" lang="ca" hreflang="ca" data-title="Formació 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-cv mw-list-item"><a href="https://cv.wikipedia.org/wiki/%C3%87%C4%83%D0%BB%D1%82%C4%83%D1%80_%D0%B9%C4%95%D1%80%D0%BA%D0%B5%D0%BB%D0%B5%D0%BD%C4%95%D0%B2%C4%95" title="Çăлтăр йĕркеленĕвĕ – Chuvash" lang="cv" hreflang="cv" data-title="Çăлтăр йĕркеленĕвĕ" data-language-autonym="Чӑвашла" data-language-local-name="Chuvash" class="interlanguage-link-target"><span>Чӑвашла</span></a></li><li class="interlanguage-link interwiki-cs mw-list-item"><a href="https://cs.wikipedia.org/wiki/Vznik_hv%C4%9Bzdy" title="Vznik hvězdy – Czech" lang="cs" hreflang="cs" data-title="Vznik hvězdy" data-language-autonym="Čeština" data-language-local-name="Czech" class="interlanguage-link-target"><span>Čeština</span></a></li><li class="interlanguage-link interwiki-de badge-Q17437798 badge-goodarticle mw-list-item" title="good article badge"><a href="https://de.wikipedia.org/wiki/Sternentstehung" title="Sternentstehung – German" lang="de" hreflang="de" data-title="Sternentstehung" data-language-autonym="Deutsch" data-language-local-name="German" class="interlanguage-link-target"><span>Deutsch</span></a></li><li class="interlanguage-link interwiki-et mw-list-item"><a href="https://et.wikipedia.org/wiki/T%C3%A4heteke" title="Täheteke – Estonian" lang="et" hreflang="et" data-title="Täheteke" data-language-autonym="Eesti" data-language-local-name="Estonian" class="interlanguage-link-target"><span>Eesti</span></a></li><li class="interlanguage-link interwiki-el mw-list-item"><a href="https://el.wikipedia.org/wiki/%CE%A3%CF%87%CE%B7%CE%BC%CE%B1%CF%84%CE%B9%CF%83%CE%BC%CF%8C%CF%82_%CF%84%CF%89%CE%BD_%CE%B1%CF%83%CF%84%CE%AD%CF%81%CF%89%CE%BD" title="Σχηματισμός των αστέρων – Greek" lang="el" hreflang="el" data-title="Σχηματισμός των αστέρων" data-language-autonym="Ελληνικά" data-language-local-name="Greek" class="interlanguage-link-target"><span>Ελληνικά</span></a></li><li class="interlanguage-link interwiki-es mw-list-item"><a href="https://es.wikipedia.org/wiki/Formaci%C3%B3n_estelar" title="Formación estelar – Spanish" lang="es" hreflang="es" data-title="Formación estelar" data-language-autonym="Español" data-language-local-name="Spanish" class="interlanguage-link-target"><span>Español</span></a></li><li class="interlanguage-link interwiki-eo mw-list-item"><a href="https://eo.wikipedia.org/wiki/Stelformado" title="Stelformado – Esperanto" lang="eo" hreflang="eo" data-title="Stelformado" data-language-autonym="Esperanto" data-language-local-name="Esperanto" class="interlanguage-link-target"><span>Esperanto</span></a></li><li class="interlanguage-link interwiki-eu mw-list-item"><a href="https://eu.wikipedia.org/wiki/Izarren_eraketa" title="Izarren eraketa – Basque" lang="eu" hreflang="eu" data-title="Izarren eraketa" data-language-autonym="Euskara" data-language-local-name="Basque" class="interlanguage-link-target"><span>Euskara</span></a></li><li class="interlanguage-link interwiki-fa mw-list-item"><a href="https://fa.wikipedia.org/wiki/%D8%B3%D8%AA%D8%A7%D8%B1%D9%87%E2%80%8C%D8%B2%D8%A7%DB%8C%DB%8C" title="ستاره‌زایی – Persian" lang="fa" hreflang="fa" data-title="ستاره‌زایی" 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/Naissance_des_%C3%A9toiles" title="Naissance des étoiles – French" lang="fr" hreflang="fr" data-title="Naissance des étoiles" data-language-autonym="Français" data-language-local-name="French" class="interlanguage-link-target"><span>Français</span></a></li><li class="interlanguage-link interwiki-gl mw-list-item"><a href="https://gl.wikipedia.org/wiki/Formaci%C3%B3n_estelar" title="Formación estelar – Galician" lang="gl" hreflang="gl" data-title="Formación estelar" data-language-autonym="Galego" data-language-local-name="Galician" class="interlanguage-link-target"><span>Galego</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_%ED%98%95%EC%84%B1" title="항성 형성 – Korean" lang="ko" hreflang="ko" data-title="항성 형성" data-language-autonym="한국어" data-language-local-name="Korean" class="interlanguage-link-target"><span>한국어</span></a></li><li class="interlanguage-link interwiki-hi mw-list-item"><a href="https://hi.wikipedia.org/wiki/%E0%A4%A4%E0%A4%BE%E0%A4%B0%E0%A4%BE_%E0%A4%A8%E0%A4%BF%E0%A4%B0%E0%A5%8D%E0%A4%AE%E0%A4%BE%E0%A4%A3" title="तारा निर्माण – Hindi" lang="hi" hreflang="hi" data-title="तारा निर्माण" data-language-autonym="हिन्दी" data-language-local-name="Hindi" class="interlanguage-link-target"><span>हिन्दी</span></a></li><li class="interlanguage-link interwiki-ig mw-list-item"><a href="https://ig.wikipedia.org/wiki/%E1%BB%8Cd%E1%BB%8Bd%E1%BB%8B_kpakpando" title="Ọdịdị kpakpando – Igbo" lang="ig" hreflang="ig" data-title="Ọdịdị kpakpando" data-language-autonym="Igbo" data-language-local-name="Igbo" class="interlanguage-link-target"><span>Igbo</span></a></li><li class="interlanguage-link interwiki-id mw-list-item"><a href="https://id.wikipedia.org/wiki/Pembentukan_bintang" title="Pembentukan bintang – Indonesian" lang="id" hreflang="id" data-title="Pembentukan 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 badge-Q17437796 badge-featuredarticle mw-list-item" title="featured article badge"><a href="https://it.wikipedia.org/wiki/Formazione_stellare" title="Formazione stellare – Italian" lang="it" hreflang="it" data-title="Formazione stellare" data-language-autonym="Italiano" data-language-local-name="Italian" class="interlanguage-link-target"><span>Italiano</span></a></li><li class="interlanguage-link interwiki-ka mw-list-item"><a href="https://ka.wikipedia.org/wiki/%E1%83%95%E1%83%90%E1%83%A0%E1%83%A1%E1%83%99%E1%83%95%E1%83%9A%E1%83%90%E1%83%95%E1%83%98%E1%83%A1_%E1%83%AC%E1%83%90%E1%83%A0%E1%83%9B%E1%83%9D%E1%83%A5%E1%83%9B%E1%83%9C%E1%83%90" title="ვარსკვლავის წარმოქმნა – Georgian" lang="ka" hreflang="ka" data-title="ვარსკვლავის წარმოქმნა" data-language-autonym="ქართული" data-language-local-name="Georgian" class="interlanguage-link-target"><span>ქართული</span></a></li><li class="interlanguage-link interwiki-lt mw-list-item"><a href="https://lt.wikipedia.org/wiki/%C5%BDvaig%C5%BEd%C4%97dara" title="Žvaigždėdara – Lithuanian" lang="lt" hreflang="lt" data-title="Žvaigždėdara" data-language-autonym="Lietuvių" data-language-local-name="Lithuanian" class="interlanguage-link-target"><span>Lietuvių</span></a></li><li class="interlanguage-link interwiki-hu mw-list-item"><a href="https://hu.wikipedia.org/wiki/Csillagkeletkez%C3%A9s" title="Csillagkeletkezés – Hungarian" lang="hu" hreflang="hu" data-title="Csillagkeletkezés" data-language-autonym="Magyar" data-language-local-name="Hungarian" class="interlanguage-link-target"><span>Magyar</span></a></li><li class="interlanguage-link interwiki-mk mw-list-item"><a href="https://mk.wikipedia.org/wiki/%D0%85%D0%B2%D0%B5%D0%B7%D0%B4%D0%BE%D0%BE%D0%B1%D1%80%D0%B0%D0%B7%D0%B1%D0%B0" title="Ѕвездообразба – Macedonian" lang="mk" hreflang="mk" data-title="Ѕвездообразба" data-language-autonym="Македонски" data-language-local-name="Macedonian" class="interlanguage-link-target"><span>Македонски</span></a></li><li class="interlanguage-link interwiki-ml mw-list-item"><a href="https://ml.wikipedia.org/wiki/%E0%B4%A8%E0%B4%95%E0%B5%8D%E0%B4%B7%E0%B4%A4%E0%B5%8D%E0%B4%B0%E0%B4%B0%E0%B5%82%E0%B4%AA%E0%B5%80%E0%B4%95%E0%B4%B0%E0%B4%A3%E0%B4%82" title="നക്ഷത്രരൂപീകരണം – Malayalam" lang="ml" hreflang="ml" data-title="നക്ഷത്രരൂപീകരണം" data-language-autonym="മലയാളം" data-language-local-name="Malayalam" class="interlanguage-link-target"><span>മലയാളം</span></a></li><li class="interlanguage-link interwiki-ms mw-list-item"><a href="https://ms.wikipedia.org/wiki/Pembentukan_bintang" title="Pembentukan bintang – Malay" lang="ms" hreflang="ms" data-title="Pembentukan 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-nl mw-list-item"><a href="https://nl.wikipedia.org/wiki/Stervorming" title="Stervorming – Dutch" lang="nl" hreflang="nl" data-title="Stervorming" data-language-autonym="Nederlands" data-language-local-name="Dutch" class="interlanguage-link-target"><span>Nederlands</span></a></li><li class="interlanguage-link interwiki-ja mw-list-item"><a href="https://ja.wikipedia.org/wiki/%E6%98%9F%E5%BD%A2%E6%88%90" title="星形成 – Japanese" lang="ja" hreflang="ja" data-title="星形成" 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/Stjernedannelse" title="Stjernedannelse – Norwegian Bokmål" lang="nb" hreflang="nb" data-title="Stjernedannelse" 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/Stjernedanning" title="Stjernedanning – Norwegian Nynorsk" lang="nn" hreflang="nn" data-title="Stjernedanning" 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-pnb mw-list-item"><a href="https://pnb.wikipedia.org/wiki/%D8%AA%D8%A7%D8%B1%DB%81_%D8%A8%D9%86%D8%AA" title="تارہ بنت – Western Punjabi" lang="pnb" hreflang="pnb" data-title="تارہ بنت" data-language-autonym="پنجابی" data-language-local-name="Western Punjabi" class="interlanguage-link-target"><span>پنجابی</span></a></li><li class="interlanguage-link interwiki-pl mw-list-item"><a href="https://pl.wikipedia.org/wiki/Powstawanie_gwiazd" title="Powstawanie gwiazd – Polish" lang="pl" hreflang="pl" data-title="Powstawanie gwiazd" data-language-autonym="Polski" data-language-local-name="Polish" class="interlanguage-link-target"><span>Polski</span></a></li><li class="interlanguage-link interwiki-pt mw-list-item"><a href="https://pt.wikipedia.org/wiki/Forma%C3%A7%C3%A3o_estelar" title="Formação estelar – Portuguese" lang="pt" hreflang="pt" data-title="Formação 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/Apari%C8%9Bia_stelelor" title="Apariția stelelor – Romanian" lang="ro" hreflang="ro" data-title="Apariția stelelor" data-language-autonym="Română" data-language-local-name="Romanian" class="interlanguage-link-target"><span>Română</span></a></li><li class="interlanguage-link interwiki-ru badge-Q17437798 badge-goodarticle mw-list-item" title="good article badge"><a href="https://ru.wikipedia.org/wiki/%D0%A4%D0%BE%D1%80%D0%BC%D0%B8%D1%80%D0%BE%D0%B2%D0%B0%D0%BD%D0%B8%D0%B5_%D0%B7%D0%B2%D0%B5%D0%B7%D0%B4%D1%8B" title="Формирование звезды – Russian" lang="ru" hreflang="ru" data-title="Формирование звезды" data-language-autonym="Русский" data-language-local-name="Russian" class="interlanguage-link-target"><span>Русский</span></a></li><li class="interlanguage-link interwiki-sq mw-list-item"><a href="https://sq.wikipedia.org/wiki/Formimi_i_yjeve" title="Formimi i yjeve – Albanian" lang="sq" hreflang="sq" data-title="Formimi i yjeve" data-language-autonym="Shqip" data-language-local-name="Albanian" class="interlanguage-link-target"><span>Shqip</span></a></li><li class="interlanguage-link interwiki-simple mw-list-item"><a href="https://simple.wikipedia.org/wiki/Star_formation" title="Star formation – Simple English" lang="en-simple" hreflang="en-simple" data-title="Star formation" data-language-autonym="Simple English" data-language-local-name="Simple English" class="interlanguage-link-target"><span>Simple English</span></a></li><li class="interlanguage-link interwiki-sk mw-list-item"><a href="https://sk.wikipedia.org/wiki/Vznik_hviezdy" title="Vznik hviezdy – Slovak" lang="sk" hreflang="sk" data-title="Vznik hviezdy" data-language-autonym="Slovenčina" data-language-local-name="Slovak" class="interlanguage-link-target"><span>Slovenčina</span></a></li><li class="interlanguage-link interwiki-sr mw-list-item"><a href="https://sr.wikipedia.org/wiki/Formiranje_zvezda" title="Formiranje zvezda – Serbian" lang="sr" 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</nav> </div> </div> </div> <div class="vector-column-end"> <div class="vector-sticky-pinned-container"> <nav class="vector-page-tools-landmark" aria-label="Page tools"> <div id="vector-page-tools-pinned-container" class="vector-pinned-container"> </div> </nav> <nav class="vector-appearance-landmark" aria-label="Appearance"> <div id="vector-appearance-pinned-container" class="vector-pinned-container"> <div id="vector-appearance" class="vector-appearance vector-pinnable-element"> <div class="vector-pinnable-header vector-appearance-pinnable-header vector-pinnable-header-pinned" data-feature-name="appearance-pinned" data-pinnable-element-id="vector-appearance" data-pinned-container-id="vector-appearance-pinned-container" data-unpinned-container-id="vector-appearance-unpinned-container" > <div class="vector-pinnable-header-label">Appearance</div> <button class="vector-pinnable-header-toggle-button vector-pinnable-header-pin-button" data-event-name="pinnable-header.vector-appearance.pin">move to sidebar</button> <button class="vector-pinnable-header-toggle-button vector-pinnable-header-unpin-button" data-event-name="pinnable-header.vector-appearance.unpin">hide</button> </div> </div> </div> </nav> </div> </div> <div id="bodyContent" class="vector-body" aria-labelledby="firstHeading" data-mw-ve-target-container> <div class="vector-body-before-content"> <div class="mw-indicators"> </div> <div 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">Process by which dense regions of molecular clouds in interstellar space collapse to form stars</div> <figure class="mw-default-size mw-halign-right" typeof="mw:File/Thumb"><a href="/wiki/File:PIA23865-W51Nebula-StarFactory-20200825.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/4/46/PIA23865-W51Nebula-StarFactory-20200825.jpg/220px-PIA23865-W51Nebula-StarFactory-20200825.jpg" decoding="async" width="220" height="124" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/4/46/PIA23865-W51Nebula-StarFactory-20200825.jpg/330px-PIA23865-W51Nebula-StarFactory-20200825.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/4/46/PIA23865-W51Nebula-StarFactory-20200825.jpg/440px-PIA23865-W51Nebula-StarFactory-20200825.jpg 2x" data-file-width="2000" data-file-height="1125" /></a><figcaption>The <a href="/w/index.php?title=Westerhout_51&action=edit&redlink=1" class="new" title="Westerhout 51 (page does not exist)">W51</a> nebula in <a href="/wiki/Aquila_(constellation)" title="Aquila (constellation)">Aquila</a> - one of the largest star factories in the Milky Way (August 25, 2020)</figcaption></figure> <p><b>Star formation</b> is the process by which dense regions within <a href="/wiki/Molecular_cloud" title="Molecular cloud">molecular clouds</a> in <a href="/wiki/Interstellar_space" class="mw-redirect" title="Interstellar space">interstellar space</a>, sometimes referred to as "stellar nurseries" or "<a href="/wiki/Star" title="Star">star</a>-forming regions", <a href="/wiki/Jeans_instability" title="Jeans instability">collapse</a> and form <a href="/wiki/Star" title="Star">stars</a>.<sup id="cite_ref-1" class="reference"><a href="#cite_note-1"><span class="cite-bracket">[</span>1<span class="cite-bracket">]</span></a></sup> As a branch of <a href="/wiki/Astronomy" title="Astronomy">astronomy</a>, star formation includes the study of the <a href="/wiki/Interstellar_medium" title="Interstellar medium">interstellar medium</a> (ISM) and <a href="/wiki/Giant_molecular_cloud" class="mw-redirect" title="Giant molecular cloud">giant molecular clouds</a> (GMC) as precursors to the star formation process, and the study of <a href="/wiki/Protostar" title="Protostar">protostars</a> and <a href="/wiki/Young_stellar_object" title="Young stellar object">young stellar objects</a> as its immediate products. It is closely related to <a href="/wiki/Planet_formation" class="mw-redirect" title="Planet formation">planet formation</a>, another branch of <a href="/wiki/Astronomy" title="Astronomy">astronomy</a>. Star formation theory, as well as accounting for the formation of a single star, must also account for the statistics of <a href="/wiki/Binary_star" title="Binary star">binary stars</a> and the <a href="/wiki/Initial_mass_function" title="Initial mass function">initial mass function</a>. Most stars do not form in isolation but as part of a group of stars referred as <a href="/wiki/Star_cluster" title="Star cluster">star clusters</a> or <a href="/wiki/Stellar_association" title="Stellar association">stellar associations</a>.<sup id="cite_ref-2" class="reference"><a href="#cite_note-2"><span class="cite-bracket">[</span>2<span class="cite-bracket">]</span></a></sup> </p> <meta property="mw:PageProp/toc" /> <div class="mw-heading mw-heading2"><h2 id="History">History</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Star_formation&action=edit&section=1" title="Edit section: History"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>The first stars were believed to be formed approximately 12-13 billion years ago following the <a href="/wiki/Big_Bang" title="Big Bang">Big Bang</a>. Over intervals of time, stars have fused helium to form a series of <a href="/wiki/Chemical_elements" class="mw-redirect" title="Chemical elements">chemical elements</a>. </p> <div class="mw-heading mw-heading2"><h2 id="Stellar_nurseries">Stellar nurseries</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Star_formation&action=edit&section=2" title="Edit section: Stellar nurseries"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <div class="mw-heading mw-heading3"><h3 id="Interstellar_clouds">Interstellar clouds</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Star_formation&action=edit&section=3" title="Edit section: Interstellar clouds"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p><a href="/wiki/Spiral_galaxy" title="Spiral galaxy">Spiral galaxies</a> like the Milky Way contain <a href="/wiki/Star" title="Star">stars</a>, <a href="/wiki/Stellar_remnant" class="mw-redirect" title="Stellar remnant">stellar remnants</a>, and a diffuse <a href="/wiki/Interstellar_medium" title="Interstellar medium">interstellar medium</a> (ISM) of gas and dust. The interstellar medium consists of 10<sup>4</sup> to 10<sup>6</sup> particles per cm<sup>3</sup>, and is typically composed of roughly 70% <a href="/wiki/Hydrogen" title="Hydrogen">hydrogen</a>, 28% <a href="/wiki/Helium" title="Helium">helium</a>, and 1.5% <a href="/wiki/Metallicity" title="Metallicity">heavier elements</a> by mass. The trace amounts of heavier elements were and are produced within stars via <a href="/wiki/Stellar_nucleosynthesis" title="Stellar nucleosynthesis">stellar nucleosynthesis</a> and ejected as the stars pass beyond the end of their <a href="/wiki/Main_sequence" title="Main sequence">main sequence</a> lifetime. Higher density regions of the interstellar medium form clouds, or <i><a href="/wiki/Diffuse_nebulae" class="mw-redirect" title="Diffuse nebulae">diffuse nebulae</a></i>,<sup id="cite_ref-3" class="reference"><a href="#cite_note-3"><span class="cite-bracket">[</span>3<span class="cite-bracket">]</span></a></sup> where star formation takes place.<sup id="cite_ref-prialnik_4-0" class="reference"><a href="#cite_note-prialnik-4"><span class="cite-bracket">[</span>4<span class="cite-bracket">]</span></a></sup> In contrast to spiral galaxies, <a href="/wiki/Elliptical_galaxy" title="Elliptical galaxy">elliptical galaxies</a> lose the cold component<sup class="noprint Inline-Template" style="white-space:nowrap;">[<i><a href="/wiki/Wikipedia:Please_clarify" title="Wikipedia:Please clarify"><span title="You can help -- (August 2023)">definition needed</span></a></i>]</sup> of its interstellar medium within roughly a billion years, which hinders the galaxy from forming diffuse nebulae except through mergers with other galaxies.<sup id="cite_ref-5" class="reference"><a href="#cite_note-5"><span class="cite-bracket">[</span>5<span class="cite-bracket">]</span></a></sup> </p> <figure class="mw-default-size mw-halign-left" typeof="mw:File/Thumb"><a href="/wiki/File:Eagle_nebula_pillars.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/b/b2/Eagle_nebula_pillars.jpg/220px-Eagle_nebula_pillars.jpg" decoding="async" width="220" height="217" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/b/b2/Eagle_nebula_pillars.jpg/330px-Eagle_nebula_pillars.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/b/b2/Eagle_nebula_pillars.jpg/440px-Eagle_nebula_pillars.jpg 2x" data-file-width="2434" data-file-height="2400" /></a><figcaption><a href="/wiki/Hubble_Space_Telescope" title="Hubble Space Telescope">Hubble Space Telescope</a> image known as <i><a href="/wiki/Pillars_of_Creation" title="Pillars of Creation">Pillars of Creation</a>,</i> where stars are forming in the <a href="/wiki/Eagle_Nebula" title="Eagle Nebula">Eagle Nebula</a></figcaption></figure> <p>In the dense nebulae where stars are produced, much of the hydrogen is in the molecular (H<sub>2</sub>) form, so these nebulae are called <a href="/wiki/Molecular_cloud" title="Molecular cloud">molecular clouds</a>.<sup id="cite_ref-prialnik_4-1" class="reference"><a href="#cite_note-prialnik-4"><span class="cite-bracket">[</span>4<span class="cite-bracket">]</span></a></sup> The <a href="/wiki/Herschel_Space_Observatory" title="Herschel Space Observatory">Herschel Space Observatory</a> has revealed that filaments, or elongated dense gas structures, are truly ubiquitous in molecular clouds and central to the star formation process. They fragment into gravitationally bound cores, most of which will evolve into stars. Continuous accretion of gas, geometrical bending<sup class="noprint Inline-Template" style="white-space:nowrap;">[<i><a href="/wiki/Wikipedia:Please_clarify" title="Wikipedia:Please clarify"><span title="You can help -- (August 2023)">definition needed</span></a></i>]</sup>, and magnetic fields may control the detailed manner in which the filaments are fragmented. Observations of supercritical filaments have revealed quasi-periodic chains of dense cores with spacing comparable to the filament inner width, and embedded protostars with outflows.<sup class="noprint Inline-Template" style="white-space:nowrap;">[<i><a href="/wiki/Wikipedia:Manual_of_Style#Technical_language" title="Wikipedia:Manual of Style"><span title="The material near this tag may be using jargon that limits the article's accessibility. (August 2023)">jargon</span></a></i>]</sup><sup id="cite_ref-6" class="reference"><a href="#cite_note-6"><span class="cite-bracket">[</span>6<span class="cite-bracket">]</span></a></sup> </p><p>Observations indicate that the coldest clouds tend to form low-mass stars, which are first observed via the infrared light they emit inside the clouds, and then as visible light when the clouds dissipate. Giant molecular clouds, which are generally warmer, produce stars of all masses.<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> These giant molecular clouds have typical densities of 100 particles per cm<sup>3</sup>, diameters of 100 <a href="/wiki/Light-year" title="Light-year">light-years</a> (9.5<span style="margin:0 .15em 0 .25em">×</span>10<sup>14</sup> <a href="/wiki/Kilometre" title="Kilometre">km</a>), masses of up to 6 million <a href="/wiki/Solar_mass" title="Solar mass">solar masses (<var>M</var><sub>☉</sub>)</a>, or six million times the mass of Earth's sun.<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> The average interior temperature is 10 <a href="/wiki/Kelvin" title="Kelvin">K</a> (−441.7 <a href="/wiki/Fahrenheit" title="Fahrenheit">°F</a>). </p><p>About half the total mass of the <a href="/wiki/Milky_Way" title="Milky Way">Milky Way</a>'s galactic ISM is found in molecular clouds<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> and the galaxy includes an estimated 6,000 molecular clouds, each with more than 100,000 <var>M</var><sub>☉</sub>.<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 nebula nearest to the <a href="/wiki/Sun" title="Sun">Sun</a> where massive stars are being formed is the <a href="/wiki/Orion_Nebula" title="Orion Nebula">Orion Nebula</a>, 1,300 light-years (1.2<span style="margin:0 .15em 0 .25em">×</span>10<sup>16</sup> km) away.<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> However, lower mass star formation is occurring about 400–450 light-years distant in the <a href="/wiki/Rho_Ophiuchi_cloud_complex" title="Rho Ophiuchi cloud complex">ρ Ophiuchi cloud complex</a>.<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> </p><p>A more compact site of star formation is the opaque clouds of dense gas and dust known as <a href="/wiki/Bok_globule" title="Bok globule">Bok globules</a>, so named after the astronomer <a href="/wiki/Bart_Bok" title="Bart Bok">Bart Bok</a>. These can form in association with collapsing molecular clouds or possibly independently.<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> The Bok globules are typically up to a light-year across and contain a few <a href="/wiki/Solar_mass" title="Solar mass">solar masses</a>.<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> They can be observed as dark clouds silhouetted against bright <a href="/wiki/Emission_nebula" title="Emission nebula">emission nebulae</a> or background stars. Over half the known Bok globules have been found to contain newly forming stars.<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> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:ALMA_witnesses_assembly_of_galaxy_in_early_Universe_(annotated).jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/9/9b/ALMA_witnesses_assembly_of_galaxy_in_early_Universe_%28annotated%29.jpg/220px-ALMA_witnesses_assembly_of_galaxy_in_early_Universe_%28annotated%29.jpg" decoding="async" width="220" height="219" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/9/9b/ALMA_witnesses_assembly_of_galaxy_in_early_Universe_%28annotated%29.jpg/330px-ALMA_witnesses_assembly_of_galaxy_in_early_Universe_%28annotated%29.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/9/9b/ALMA_witnesses_assembly_of_galaxy_in_early_Universe_%28annotated%29.jpg/440px-ALMA_witnesses_assembly_of_galaxy_in_early_Universe_%28annotated%29.jpg 2x" data-file-width="2000" data-file-height="1990" /></a><figcaption>Assembly of galaxy in early Universe.<sup id="cite_ref-16" class="reference"><a href="#cite_note-16"><span class="cite-bracket">[</span>16<span class="cite-bracket">]</span></a></sup></figcaption></figure> <div class="mw-heading mw-heading3"><h3 id="Cloud_collapse">Cloud collapse</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Star_formation&action=edit&section=4" title="Edit section: Cloud collapse"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>An interstellar cloud of gas will remain in <a href="/wiki/Hydrostatic_equilibrium" title="Hydrostatic equilibrium">hydrostatic equilibrium</a> as long as the <a href="/wiki/Kinetic_energy" title="Kinetic energy">kinetic energy</a> of the gas <a href="/wiki/Pressure" title="Pressure">pressure</a> is in balance with the <a href="/wiki/Potential_energy" title="Potential energy">potential energy</a> of the internal <a href="/wiki/Gravitational_force" class="mw-redirect" title="Gravitational force">gravitational force</a>. Mathematically this is expressed using the <a href="/wiki/Virial_theorem" title="Virial theorem">virial theorem</a>, which states that, to maintain equilibrium, the gravitational potential energy must equal twice the internal thermal energy.<sup id="cite_ref-17" class="reference"><a href="#cite_note-17"><span class="cite-bracket">[</span>17<span class="cite-bracket">]</span></a></sup> If a cloud is massive enough that the gas pressure is insufficient to support it, the cloud will undergo <a href="/wiki/Gravitational_collapse" title="Gravitational collapse">gravitational collapse</a>. The mass above which a cloud will undergo such collapse is called the <a href="/wiki/Jeans_mass" class="mw-redirect" title="Jeans mass">Jeans mass</a>. The Jeans mass depends on the temperature and density of the cloud, but is typically thousands to tens of thousands of solar masses.<sup id="cite_ref-prialnik_4-2" class="reference"><a href="#cite_note-prialnik-4"><span class="cite-bracket">[</span>4<span class="cite-bracket">]</span></a></sup> During cloud collapse dozens to tens of thousands of stars form more or less simultaneously which is observable in so-called <a href="/wiki/Embedded_cluster" title="Embedded cluster">embedded clusters</a>. The end product of a core collapse is an <a href="/wiki/Open_cluster" title="Open cluster">open cluster</a> of stars.<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> </p> <figure class="mw-default-size mw-halign-left" typeof="mw:File/Thumb"><a href="/wiki/File:ALMA_views_a_stellar_explosion_in_Orion.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/5/56/ALMA_views_a_stellar_explosion_in_Orion.jpg/220px-ALMA_views_a_stellar_explosion_in_Orion.jpg" decoding="async" width="220" height="229" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/5/56/ALMA_views_a_stellar_explosion_in_Orion.jpg/330px-ALMA_views_a_stellar_explosion_in_Orion.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/5/56/ALMA_views_a_stellar_explosion_in_Orion.jpg/440px-ALMA_views_a_stellar_explosion_in_Orion.jpg 2x" data-file-width="1280" data-file-height="1335" /></a><figcaption><a href="/wiki/Atacama_Large_Millimeter_Array" title="Atacama Large Millimeter Array">ALMA</a> observations of the Orion Nebula complex provide insights into explosions at star birth.<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></figcaption></figure> <p>In <i>triggered star formation</i>, one of several events might occur to compress a molecular cloud and initiate its <a href="/wiki/Gravitational_collapse" title="Gravitational collapse">gravitational collapse</a>. Molecular clouds may collide with each other, or a nearby <a href="/wiki/Supernova" title="Supernova">supernova</a> explosion can be a trigger, sending <a href="/wiki/Shock_wave" title="Shock wave">shocked</a> matter into the cloud at very high speeds.<sup id="cite_ref-prialnik_4-3" class="reference"><a href="#cite_note-prialnik-4"><span class="cite-bracket">[</span>4<span class="cite-bracket">]</span></a></sup> (The resulting new stars may themselves soon produce supernovae, producing <a href="/wiki/SSPSF_model" title="SSPSF model">self-propagating star formation</a>.) Alternatively, <a href="/wiki/Interacting_galaxy" title="Interacting galaxy">galactic collisions</a> can trigger massive <a href="/wiki/Starburst_(astronomy)" class="mw-redirect" title="Starburst (astronomy)">starbursts</a> of star formation as the gas clouds in each galaxy are compressed and agitated by <a href="/wiki/Galactic_tide" title="Galactic tide">tidal forces</a>.<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> The latter mechanism may be responsible for the formation of <a href="/wiki/Globular_cluster" title="Globular cluster">globular clusters</a>.<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> </p><p>A <a href="/wiki/Supermassive_black_hole" title="Supermassive black hole">supermassive black hole</a> at the core of a galaxy may serve to regulate the rate of star formation in a galactic nucleus. A black hole that is accreting infalling matter can become <a href="/wiki/Active_galactic_nucleus" title="Active galactic nucleus">active</a>, emitting a strong wind through a collimated <a href="/wiki/Relativistic_jet" class="mw-redirect" title="Relativistic jet">relativistic jet</a>. This can limit further star formation. Massive black holes ejecting radio-frequency-emitting particles at near-light speed can also block the formation of new stars in aging galaxies.<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> However, the radio emissions around the jets may also trigger star formation. Likewise, a weaker jet may trigger star formation when it collides with a cloud.<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> </p> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Size_can_be_deceptive_ESO_553-46.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/3/3a/Size_can_be_deceptive_ESO_553-46.jpg/220px-Size_can_be_deceptive_ESO_553-46.jpg" decoding="async" width="220" height="110" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/3/3a/Size_can_be_deceptive_ESO_553-46.jpg/330px-Size_can_be_deceptive_ESO_553-46.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/3/3a/Size_can_be_deceptive_ESO_553-46.jpg/440px-Size_can_be_deceptive_ESO_553-46.jpg 2x" data-file-width="1280" data-file-height="638" /></a><figcaption>Dwarf galaxy <a href="/w/index.php?title=ESO_553-46&action=edit&redlink=1" class="new" title="ESO 553-46 (page does not exist)">ESO 553-46</a> has one of the highest rates of star formation of the 1000 or so galaxies nearest to the Milky Way.<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></figcaption></figure> <p>As it collapses, a molecular cloud breaks into smaller and smaller pieces in a hierarchical manner, until the fragments reach stellar mass. In each of these fragments, the collapsing gas radiates away the energy gained by the release of <a href="/wiki/Gravitational" class="mw-redirect" title="Gravitational">gravitational</a> <a href="/wiki/Potential_energy" title="Potential energy">potential energy</a>. As the density increases, the fragments become opaque and are thus less efficient at radiating away their energy. This raises the temperature of the cloud and inhibits further fragmentation. The fragments now condense into rotating spheres of gas that serve as stellar embryos.<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> </p><p>Complicating this picture of a collapsing cloud are the effects of <a href="/wiki/Turbulence" title="Turbulence">turbulence</a>, macroscopic flows, <a href="/wiki/Rotation" title="Rotation">rotation</a>, <a href="/wiki/Magnetic_fields" class="mw-redirect" title="Magnetic fields">magnetic fields</a> and the cloud geometry. Both rotation and magnetic fields can hinder the collapse of a cloud.<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><sup id="cite_ref-27" class="reference"><a href="#cite_note-27"><span class="cite-bracket">[</span>27<span class="cite-bracket">]</span></a></sup> Turbulence is instrumental in causing fragmentation of the cloud, and on the smallest scales it promotes collapse.<sup id="cite_ref-28" class="reference"><a href="#cite_note-28"><span class="cite-bracket">[</span>28<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading2"><h2 id="Protostar">Protostar</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Star_formation&action=edit&section=5" title="Edit section: Protostar"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></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">Main article: <a href="/wiki/Protostar" title="Protostar">Protostar</a></div> <figure class="mw-default-size mw-halign-right" typeof="mw:File/Thumb"><a href="/wiki/File:LH_95.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/8/87/LH_95.jpg/220px-LH_95.jpg" decoding="async" width="220" height="235" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/8/87/LH_95.jpg/330px-LH_95.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/8/87/LH_95.jpg/440px-LH_95.jpg 2x" data-file-width="3622" data-file-height="3877" /></a><figcaption><a href="/wiki/LH_95" title="LH 95">LH 95</a> stellar nursery in Large Magellanic Cloud.</figcaption></figure> <p>A protostellar cloud will continue to collapse as long as the gravitational binding energy can be eliminated. This excess energy is primarily lost through radiation. However, the collapsing cloud will eventually become opaque to its own radiation, and the energy must be removed through some other means. The dust within the cloud becomes heated to temperatures of <span class="nowrap">60–100 K</span>, and these particles radiate at wavelengths in the far infrared where the cloud is transparent. Thus the dust mediates the further collapse of the cloud.<sup id="cite_ref-29" class="reference"><a href="#cite_note-29"><span class="cite-bracket">[</span>29<span class="cite-bracket">]</span></a></sup> </p><p>During the collapse, the density of the cloud increases towards the center and thus the middle region becomes optically opaque first. This occurs when the density is about <span class="nowrap">10<sup>−13</sup> g / cm<sup>3</sup></span>. A core region, called the first hydrostatic core, forms where the collapse is essentially halted. It continues to increase in temperature as determined by the virial theorem. The gas falling toward this opaque region collides with it and creates shock waves that further heat the core.<sup id="cite_ref-larson_30-0" class="reference"><a href="#cite_note-larson-30"><span class="cite-bracket">[</span>30<span class="cite-bracket">]</span></a></sup> </p> <figure class="mw-default-size mw-halign-left" typeof="mw:File/Thumb"><a href="/wiki/File:Cepheus_B.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/4/4a/Cepheus_B.jpg/220px-Cepheus_B.jpg" decoding="async" width="220" height="165" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/4/4a/Cepheus_B.jpg/330px-Cepheus_B.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/4/4a/Cepheus_B.jpg/440px-Cepheus_B.jpg 2x" data-file-width="1432" data-file-height="1074" /></a><figcaption><a href="/wiki/Composite_image" class="mw-redirect" title="Composite image">Composite image</a> showing young stars in and around molecular cloud <a href="/wiki/Cepheus_(constellation)" title="Cepheus (constellation)">Cepheus</a> B.</figcaption></figure> <p>When the core temperature reaches about <span class="nowrap">2000 K</span>, the thermal energy dissociates the H<sub>2</sub> molecules.<sup id="cite_ref-larson_30-1" class="reference"><a href="#cite_note-larson-30"><span class="cite-bracket">[</span>30<span class="cite-bracket">]</span></a></sup> This is followed by the ionization of the hydrogen and helium atoms. These processes absorb the energy of the contraction, allowing it to continue on timescales comparable to the period of collapse at free fall velocities.<sup id="cite_ref-31" class="reference"><a href="#cite_note-31"><span class="cite-bracket">[</span>31<span class="cite-bracket">]</span></a></sup> After the density of infalling material has reached about 10<sup>−8</sup> g / cm<sup>3</sup>, that material is sufficiently transparent to allow energy radiated by the protostar to escape. The combination of convection within the protostar and radiation from its exterior allow the star to contract further.<sup id="cite_ref-larson_30-2" class="reference"><a href="#cite_note-larson-30"><span class="cite-bracket">[</span>30<span class="cite-bracket">]</span></a></sup> This continues until the gas is hot enough for the internal <a href="/wiki/Pressure" title="Pressure">pressure</a> to support the protostar against further gravitational collapse—a state called <a href="/wiki/Hydrostatic_equilibrium" title="Hydrostatic equilibrium">hydrostatic equilibrium</a>. When this accretion phase is nearly complete, the resulting object is known as a <a href="/wiki/Protostar" title="Protostar">protostar</a>.<sup id="cite_ref-prialnik_4-4" class="reference"><a href="#cite_note-prialnik-4"><span class="cite-bracket">[</span>4<span class="cite-bracket">]</span></a></sup> </p> <figure class="mw-default-size mw-halign-right" typeof="mw:File/Thumb"><a href="/wiki/File:N11_(Hubble).jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/0/0b/N11_%28Hubble%29.jpg/220px-N11_%28Hubble%29.jpg" decoding="async" width="220" height="216" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/0/0b/N11_%28Hubble%29.jpg/330px-N11_%28Hubble%29.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/0/0b/N11_%28Hubble%29.jpg/440px-N11_%28Hubble%29.jpg 2x" data-file-width="7546" data-file-height="7418" /></a><figcaption> N11, part of a complex network of gas clouds and star clusters within our neighbouring galaxy, the Large Magellanic Cloud.</figcaption></figure> <p>Accretion of material onto the protostar continues partially from the newly formed <a href="/wiki/Circumstellar_disc" title="Circumstellar disc">circumstellar disc</a>. When the density and temperature are high enough, <a href="/wiki/Deuterium_fusion" title="Deuterium fusion">deuterium fusion</a> begins, and the outward <a href="/wiki/Radiation_pressure" title="Radiation pressure">pressure</a> of the resultant radiation slows (but does not stop) the collapse. Material comprising the cloud continues to "rain" onto the <a href="/wiki/Protostar" title="Protostar">protostar</a>. In this stage bipolar jets are produced called <a href="/wiki/Herbig%E2%80%93Haro_object" title="Herbig–Haro object">Herbig–Haro objects</a>. This is probably the means by which excess <a href="/wiki/Angular_momentum" title="Angular momentum">angular momentum</a> of the infalling material is expelled, allowing the star to continue to form. </p> <figure class="mw-default-size mw-halign-left" typeof="mw:File/Thumb"><a href="/wiki/File:Star_formation_region_Lupus_3.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/f/fb/Star_formation_region_Lupus_3.jpg/220px-Star_formation_region_Lupus_3.jpg" decoding="async" width="220" height="139" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/f/fb/Star_formation_region_Lupus_3.jpg/330px-Star_formation_region_Lupus_3.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/f/fb/Star_formation_region_Lupus_3.jpg/440px-Star_formation_region_Lupus_3.jpg 2x" data-file-width="18000" data-file-height="11360" /></a><figcaption>Star formation region <a href="/w/index.php?title=Lupus_3&action=edit&redlink=1" class="new" title="Lupus 3 (page does not exist)">Lupus 3</a>.<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></figcaption></figure> <p>When the surrounding gas and dust envelope disperses and accretion process stops, the star is considered a <a href="/wiki/Pre-main-sequence_star" title="Pre-main-sequence star">pre-main-sequence star</a> (PMS star). The energy source of these objects is (gravitational contraction)<a href="/wiki/Kelvin%E2%80%93Helmholtz_mechanism" title="Kelvin–Helmholtz mechanism">Kelvin–Helmholtz mechanism</a>, as opposed to hydrogen burning in main sequence stars. The PMS star follows a <a href="/wiki/Hayashi_track" title="Hayashi track">Hayashi track</a> on the <a href="/wiki/Hertzsprung%E2%80%93Russell_diagram" title="Hertzsprung–Russell diagram">Hertzsprung–Russell (H–R) diagram</a>.<sup id="cite_ref-33" class="reference"><a href="#cite_note-33"><span class="cite-bracket">[</span>33<span class="cite-bracket">]</span></a></sup> The contraction will proceed until the <a href="/wiki/Hayashi_limit" title="Hayashi limit">Hayashi limit</a> is reached, and thereafter contraction will continue on a <a href="/wiki/Kelvin%E2%80%93Helmholtz_mechanism" title="Kelvin–Helmholtz mechanism">Kelvin–Helmholtz timescale</a> with the temperature remaining stable. Stars with less than 0.5 <var>M</var><sub>☉</sub> thereafter join the main sequence. For more massive PMS stars, at the end of the Hayashi track they will slowly collapse in near hydrostatic equilibrium, following the <a href="/wiki/Henyey_track" title="Henyey track">Henyey track</a>.<sup id="cite_ref-34" class="reference"><a href="#cite_note-34"><span class="cite-bracket">[</span>34<span class="cite-bracket">]</span></a></sup> </p><p>Finally, <a href="/wiki/Hydrogen" title="Hydrogen">hydrogen</a> begins to fuse in the core of the star, and the rest of the enveloping material is cleared away. This ends the protostellar phase and begins the star's <a href="/wiki/Main_sequence" title="Main sequence">main sequence</a> phase on the H–R diagram. </p><p>The stages of the process are well defined in stars with masses around 1 <var>M</var><sub>☉</sub> or less. In high mass stars, the length of the star formation process is comparable to the other timescales of their evolution, much shorter, and the process is not so well defined. The later evolution of stars is studied in <a href="/wiki/Stellar_evolution" title="Stellar evolution">stellar evolution</a>. </p> <table class="wikitable" style="margin:0.5em auto; width:600px;"> <tbody><tr> <th><a href="/wiki/Protostar" title="Protostar">Protostar</a> </th></tr> <tr> <td style="font-size:88%"><span typeof="mw:File"><a href="/wiki/File:PIA18928-Protostar-HOPS383-20150323.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/8/83/PIA18928-Protostar-HOPS383-20150323.jpg/600px-PIA18928-Protostar-HOPS383-20150323.jpg" decoding="async" width="600" height="338" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/8/83/PIA18928-Protostar-HOPS383-20150323.jpg/900px-PIA18928-Protostar-HOPS383-20150323.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/8/83/PIA18928-Protostar-HOPS383-20150323.jpg/1200px-PIA18928-Protostar-HOPS383-20150323.jpg 2x" data-file-width="4008" data-file-height="2255" /></a></span> <div class="center" style="width:auto; margin-left:auto; margin-right:auto;">Protostar outburst - <a href="/wiki/HOPS_383" title="HOPS 383">HOPS 383</a> (2015).</div> </td></tr></tbody></table> <div class="mw-heading mw-heading2"><h2 id="Observations">Observations</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Star_formation&action=edit&section=6" title="Edit section: Observations"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size mw-halign-left" typeof="mw:File/Thumb"><a href="/wiki/File:Orion_Nebula_-_Hubble_2006_mosaic_18000.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/f/f3/Orion_Nebula_-_Hubble_2006_mosaic_18000.jpg/220px-Orion_Nebula_-_Hubble_2006_mosaic_18000.jpg" decoding="async" width="220" height="220" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/f/f3/Orion_Nebula_-_Hubble_2006_mosaic_18000.jpg/330px-Orion_Nebula_-_Hubble_2006_mosaic_18000.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/f/f3/Orion_Nebula_-_Hubble_2006_mosaic_18000.jpg/440px-Orion_Nebula_-_Hubble_2006_mosaic_18000.jpg 2x" data-file-width="18000" data-file-height="18000" /></a><figcaption>The <a href="/wiki/Orion_Nebula" title="Orion Nebula">Orion Nebula</a> is an archetypical example of star formation, from the massive, young stars that are shaping the nebula to the pillars of dense gas that may be the homes of budding stars.</figcaption></figure> <p>Key elements of star formation are only available by observing in <a href="/wiki/Wavelength" title="Wavelength">wavelengths</a> other than the <a href="/wiki/Visible-light_astronomy" title="Visible-light astronomy">optical</a>. The protostellar stage of stellar existence is almost invariably hidden away deep inside dense clouds of gas and dust left over from the <a href="/wiki/Giant_molecular_cloud" class="mw-redirect" title="Giant molecular cloud">GMC</a>. Often, these star-forming cocoons known as <a href="/wiki/Bok_globule" title="Bok globule">Bok globules</a>, can be seen in <a href="/wiki/Silhouette" title="Silhouette">silhouette</a> against bright emission from surrounding gas.<sup id="cite_ref-35" class="reference"><a href="#cite_note-35"><span class="cite-bracket">[</span>35<span class="cite-bracket">]</span></a></sup> Early stages of a star's life can be seen in <a href="/wiki/Infrared_astronomy" title="Infrared astronomy">infrared</a> light, which penetrates the dust more easily than <a href="/wiki/Visible-light_astronomy" title="Visible-light astronomy">visible</a> light.<sup id="cite_ref-36" class="reference"><a href="#cite_note-36"><span class="cite-bracket">[</span>36<span class="cite-bracket">]</span></a></sup> Observations from the <a href="/wiki/Wide-field_Infrared_Survey_Explorer" title="Wide-field Infrared Survey Explorer">Wide-field Infrared Survey Explorer</a> (WISE) have thus been especially important for unveiling numerous galactic protostars and their parent <a href="/wiki/Star_cluster" title="Star cluster">star clusters</a>.<sup id="cite_ref-wright_37-0" class="reference"><a href="#cite_note-wright-37"><span class="cite-bracket">[</span>37<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-ma2013_38-0" class="reference"><a href="#cite_note-ma2013-38"><span class="cite-bracket">[</span>38<span class="cite-bracket">]</span></a></sup> Examples of such embedded star clusters are FSR 1184, FSR 1190, Camargo 14, Camargo 74, Majaess 64, and Majaess 98.<sup id="cite_ref-ca2015_39-0" class="reference"><a href="#cite_note-ca2015-39"><span class="cite-bracket">[</span>39<span class="cite-bracket">]</span></a></sup> </p> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Star-forming_region_S106_(captured_by_the_Hubble_Space_Telescope).jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/c/ca/Star-forming_region_S106_%28captured_by_the_Hubble_Space_Telescope%29.jpg/220px-Star-forming_region_S106_%28captured_by_the_Hubble_Space_Telescope%29.jpg" decoding="async" width="220" height="162" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/c/ca/Star-forming_region_S106_%28captured_by_the_Hubble_Space_Telescope%29.jpg/330px-Star-forming_region_S106_%28captured_by_the_Hubble_Space_Telescope%29.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/c/ca/Star-forming_region_S106_%28captured_by_the_Hubble_Space_Telescope%29.jpg/440px-Star-forming_region_S106_%28captured_by_the_Hubble_Space_Telescope%29.jpg 2x" data-file-width="4356" data-file-height="3202" /></a><figcaption>Star-forming region S106.</figcaption></figure> <p>The structure of the molecular cloud and the effects of the protostar can be observed in near-IR <a href="/wiki/Extinction_(astronomy)" title="Extinction (astronomy)">extinction</a> maps (where the number of stars are counted per unit area and compared to a nearby zero extinction area of sky), continuum dust emission and <a href="/wiki/Rotational_transition" title="Rotational transition">rotational transitions</a> of <a href="/wiki/Carbon_monoxide" title="Carbon monoxide">CO</a> and other molecules; these last two are observed in the millimeter and <a href="/wiki/Radio_astronomy" title="Radio astronomy">submillimeter</a> range. The radiation from the protostar and early star has to be observed in <a href="/wiki/Infrared" title="Infrared">infrared astronomy</a> wavelengths, as the <a href="/wiki/Extinction_(astronomy)" title="Extinction (astronomy)">extinction</a> caused by the rest of the cloud in which the star is forming is usually too big to allow us to observe it in the visual part of the spectrum. This presents considerable difficulties as the Earth's atmosphere is almost entirely opaque from 20μm to 850μm, with narrow windows at 200μm and 450μm. Even outside this range, atmospheric subtraction techniques must be used. </p> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:NASA-FlameNebula-NGC2024-20140507.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/3/36/NASA-FlameNebula-NGC2024-20140507.jpg/220px-NASA-FlameNebula-NGC2024-20140507.jpg" decoding="async" width="220" height="220" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/3/36/NASA-FlameNebula-NGC2024-20140507.jpg/330px-NASA-FlameNebula-NGC2024-20140507.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/3/36/NASA-FlameNebula-NGC2024-20140507.jpg/440px-NASA-FlameNebula-NGC2024-20140507.jpg 2x" data-file-width="3600" data-file-height="3600" /></a><figcaption>Young stars (purple) revealed by X-ray inside the <a href="/wiki/Flame_Nebula" title="Flame Nebula">NGC 2024</a> star-forming region.<sup id="cite_ref-Getman14_40-0" class="reference"><a href="#cite_note-Getman14-40"><span class="cite-bracket">[</span>40<span class="cite-bracket">]</span></a></sup></figcaption></figure> <p><a href="/wiki/X-ray_astronomy" title="X-ray astronomy">X-ray</a> observations have proven useful for studying young stars, since X-ray emission from these objects is about 100–100,000 times stronger than X-ray emission from main-sequence stars.<sup id="cite_ref-Preibisch05_41-0" class="reference"><a href="#cite_note-Preibisch05-41"><span class="cite-bracket">[</span>41<span class="cite-bracket">]</span></a></sup> The earliest detections of X-rays from T Tauri stars were made by the <a href="/wiki/Einstein_Observatory" title="Einstein Observatory">Einstein X-ray Observatory</a>.<sup id="cite_ref-Feigelson81_42-0" class="reference"><a href="#cite_note-Feigelson81-42"><span class="cite-bracket">[</span>42<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-Montmerle83_43-0" class="reference"><a href="#cite_note-Montmerle83-43"><span class="cite-bracket">[</span>43<span class="cite-bracket">]</span></a></sup> For low-mass stars X-rays are generated by the heating of the stellar corona through <a href="/wiki/Magnetic_reconnection" title="Magnetic reconnection">magnetic reconnection</a>, while for high-mass <a href="/wiki/O-type_star" title="O-type star">O</a> and early B-type stars X-rays are generated through supersonic shocks in the stellar winds. Photons in the soft X-ray energy range covered by the <a href="/wiki/Chandra_X-ray_Observatory" title="Chandra X-ray Observatory">Chandra X-ray Observatory</a> and <a href="/wiki/XMM-Newton" title="XMM-Newton">XMM-Newton</a> may penetrate the interstellar medium with only moderate absorption due to gas, making the X-ray a useful wavelength for seeing the stellar populations within molecular clouds. X-ray emission as evidence of stellar youth makes this band particularly useful for performing censuses of stars in star-forming regions, given that not all young stars have infrared excesses.<sup id="cite_ref-feigelson13_44-0" class="reference"><a href="#cite_note-feigelson13-44"><span class="cite-bracket">[</span>44<span class="cite-bracket">]</span></a></sup> X-ray observations have provided near-complete censuses of all stellar-mass objects in the <a href="/wiki/Orion_Nebula" title="Orion Nebula">Orion Nebula Cluster</a> and <a href="/wiki/Taurus_Molecular_Cloud" class="mw-redirect" title="Taurus Molecular Cloud">Taurus Molecular Cloud</a>.<sup id="cite_ref-Getman05_45-0" class="reference"><a href="#cite_note-Getman05-45"><span class="cite-bracket">[</span>45<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-Gudel07_46-0" class="reference"><a href="#cite_note-Gudel07-46"><span class="cite-bracket">[</span>46<span class="cite-bracket">]</span></a></sup> </p><p>The formation of individual stars can only be directly observed in the <a href="/wiki/Milky_Way" title="Milky Way">Milky Way Galaxy</a>, but in distant galaxies star formation has been detected through its unique <a href="/wiki/Gas_chromatography%E2%80%93mass_spectrometry" title="Gas chromatography–mass spectrometry">spectral signature</a>. </p><p>Initial research indicates star-forming clumps start as giant, dense areas in turbulent gas-rich matter in young galaxies, live about 500 million years, and may migrate to the center of a galaxy, creating the central bulge of a galaxy.<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><p>On February 21, 2014, <a href="/wiki/NASA" title="NASA">NASA</a> announced a <a rel="nofollow" class="external text" href="http://www.astrochem.org/pahdb/">greatly upgraded database</a> for tracking <a href="/wiki/Polycyclic_aromatic_hydrocarbon" title="Polycyclic aromatic hydrocarbon">polycyclic aromatic hydrocarbons</a> (PAHs) in the <a href="/wiki/Universe" title="Universe">universe</a>. According to scientists, more than 20% of the <a href="/wiki/Carbon" title="Carbon">carbon</a> in the universe may be associated with PAHs, possible <a href="/wiki/PAH_world_hypothesis" title="PAH world hypothesis">starting materials</a> for the <a href="/wiki/Abiogenesis#PAH_world_hypothesis" title="Abiogenesis">formation</a> of <a href="/wiki/Life#Extraterrestrial" title="Life">life</a>. PAHs seem to have been formed shortly after the <a href="/wiki/Big_Bang" title="Big Bang">Big Bang</a>, are widespread throughout the universe, and are associated with new stars and <a href="/wiki/Exoplanet" title="Exoplanet">exoplanets</a>.<sup id="cite_ref-NASA-201409221_48-0" class="reference"><a href="#cite_note-NASA-201409221-48"><span class="cite-bracket">[</span>48<span class="cite-bracket">]</span></a></sup> </p><p>In February 2018, astronomers reported, for the first time, a signal of the <a href="/wiki/Reionization" title="Reionization">reionization</a> epoch, an indirect detection of light from the earliest stars formed - about 180 million years after the <a href="/wiki/Big_Bang" title="Big Bang">Big Bang</a>.<sup id="cite_ref-NAT-20180228_49-0" class="reference"><a href="#cite_note-NAT-20180228-49"><span class="cite-bracket">[</span>49<span class="cite-bracket">]</span></a></sup> </p><p>An article published on October 22, 2019, reported on the detection of <a href="/wiki/3MM-1" title="3MM-1">3MM-1</a>, a massive star-forming galaxy about 12.5 billion light-years away that is obscured by clouds of <a href="/wiki/Cosmic_dust" title="Cosmic dust">dust</a>.<sup id="cite_ref-WilliamsLabbe2019_50-0" class="reference"><a href="#cite_note-WilliamsLabbe2019-50"><span class="cite-bracket">[</span>50<span class="cite-bracket">]</span></a></sup> At a mass of about 10<sup>10.8</sup> <a href="/wiki/Solar_mass" title="Solar mass">solar masses</a>, it showed a star formation rate about 100 times as high as in the <a href="/wiki/Milky_Way" title="Milky Way">Milky Way</a>.<sup id="cite_ref-UAnews_51-0" class="reference"><a href="#cite_note-UAnews-51"><span class="cite-bracket">[</span>51<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading3"><h3 id="Notable_pathfinder_objects">Notable pathfinder objects</h3><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Star_formation&action=edit&section=7" title="Edit section: Notable pathfinder objects"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <ul><li><a href="/wiki/MWC_349" title="MWC 349">MWC 349</a> was first discovered in 1978, and is estimated to be only 1,000 years old.</li> <li>VLA 1623 – The first exemplar Class 0 protostar, a type of embedded protostar that has yet to accrete the majority of its mass. Found in 1993, is possibly younger than 10,000 years.<sup id="cite_ref-AndreWard-Thompson1993_52-0" class="reference"><a href="#cite_note-AndreWard-Thompson1993-52"><span class="cite-bracket">[</span>52<span class="cite-bracket">]</span></a></sup></li> <li><a href="/wiki/L1014" title="L1014">L1014</a> – An extremely faint embedded object representative of a new class of sources that are only now being detected with the newest telescopes. Their status is still undetermined, they could be the youngest low-mass Class 0 protostars yet seen or even very low-mass evolved objects (like <a href="/wiki/Brown_dwarf" title="Brown dwarf">brown dwarfs</a> or even <a href="/wiki/Rogue_planet" title="Rogue planet">rogue planets</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></li> <li><a href="/wiki/GCIRS_8*" title="GCIRS 8*">GCIRS 8*</a> – The youngest known <a href="/wiki/Main_sequence" title="Main sequence">main sequence</a> star in the <a href="/wiki/Galactic_Center" title="Galactic Center">Galactic Center</a> region, discovered in August 2006. It is estimated to be 3.5 million years old.<sup id="cite_ref-GeballeNajarro2006_54-0" class="reference"><a href="#cite_note-GeballeNajarro2006-54"><span class="cite-bracket">[</span>54<span class="cite-bracket">]</span></a></sup></li></ul> <div class="mw-heading mw-heading2"><h2 id="Low_mass_and_high_mass_star_formation">Low mass and high mass star formation</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Star_formation&action=edit&section=8" title="Edit section: Low mass and high mass star formation"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:Infrared_Image_of_Dark_Cloud_in_Aquila.jpg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/1/13/Infrared_Image_of_Dark_Cloud_in_Aquila.jpg/220px-Infrared_Image_of_Dark_Cloud_in_Aquila.jpg" decoding="async" width="220" height="220" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/1/13/Infrared_Image_of_Dark_Cloud_in_Aquila.jpg/330px-Infrared_Image_of_Dark_Cloud_in_Aquila.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/1/13/Infrared_Image_of_Dark_Cloud_in_Aquila.jpg/440px-Infrared_Image_of_Dark_Cloud_in_Aquila.jpg 2x" data-file-width="1930" data-file-height="1930" /></a><figcaption>Star-forming region <a href="/wiki/Westerhout_40" title="Westerhout 40">Westerhout 40</a> and the <a href="/wiki/Serpens-Aquila_Rift" class="mw-redirect" title="Serpens-Aquila Rift">Serpens-Aquila Rift</a>- cloud filaments containing new stars fill the region.<sup id="cite_ref-kuhn10_55-0" class="reference"><a href="#cite_note-kuhn10-55"><span class="cite-bracket">[</span>55<span class="cite-bracket">]</span></a></sup><sup id="cite_ref-andre10_56-0" class="reference"><a href="#cite_note-andre10-56"><span class="cite-bracket">[</span>56<span class="cite-bracket">]</span></a></sup> </figcaption></figure> <p>Stars of different masses are thought to form by slightly different mechanisms. The theory of low-mass star formation, which is well-supported by observation, suggests that low-mass stars form by the gravitational collapse of rotating density enhancements within molecular clouds. As described above, the collapse of a rotating cloud of gas and dust leads to the formation of an accretion disk through which matter is channeled onto a central protostar. For stars with masses higher than about 8 <var>M</var><sub>☉</sub>, however, the mechanism of star formation is not well understood. </p><p>Massive stars emit copious quantities of radiation which pushes against infalling material. In the past, it was thought that this <a href="/wiki/Radiation_pressure" title="Radiation pressure">radiation pressure</a> might be substantial enough to halt accretion onto the massive protostar and prevent the formation of stars with masses more than a few tens of solar masses.<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> Recent theoretical work has shown that the production of a jet and outflow clears a cavity through which much of the radiation from a massive protostar can escape without hindering accretion through the disk and onto the protostar.<sup id="cite_ref-58" class="reference"><a href="#cite_note-58"><span class="cite-bracket">[</span>58<span class="cite-bracket">]</span></a></sup><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> Present thinking is that massive stars may therefore be able to form by a mechanism similar to that by which low mass stars form. </p><p>There is mounting evidence that at least some massive protostars are indeed surrounded by accretion disks.<sup id="cite_ref-rab_60-0" class="reference"><a href="#cite_note-rab-60"><span class="cite-bracket">[</span>60<span class="cite-bracket">]</span></a></sup> Disk accretion in high-mass protostars, similar to their low-mass counterparts, is expected to exhibit bursts of episodic accretion as a result of a gravitationally instability leading to clumpy and in-continuous accretion rates. Recent evidence of accretion bursts in high-mass protostars has indeed been confirmed observationally.<sup id="cite_ref-rab_60-1" class="reference"><a href="#cite_note-rab-60"><span class="cite-bracket">[</span>60<span class="cite-bracket">]</span></a></sup><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><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> Several other theories of massive star formation remain to be tested observationally. Of these, perhaps the most prominent is the theory of competitive accretion, which suggests that massive protostars are "seeded" by low-mass protostars which compete with other protostars to draw in matter from the entire parent molecular cloud, instead of simply from a small local region.<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><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><p>Another theory of massive star formation suggests that massive stars may form by the coalescence of two or more stars of lower mass.<sup id="cite_ref-65" class="reference"><a href="#cite_note-65"><span class="cite-bracket">[</span>65<span class="cite-bracket">]</span></a></sup> </p> <div class="mw-heading mw-heading2"><h2 id="Filamentary_nature_of_star_formation">Filamentary nature of star formation</h2><span class="mw-editsection"><span class="mw-editsection-bracket">[</span><a href="/w/index.php?title=Star_formation&action=edit&section=9" title="Edit section: Filamentary nature of star formation"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <p>Recent studies have emphasized the role of filamentary structures in molecular clouds as the initial conditions for star formation. Findings from the Herschel Space Observatory highlight the ubiquitous nature of these filaments in the cold interstellar medium (ISM). The spatial relationship between cores and filaments indicates that the majority of prestellar cores are located within 0.1 pc of supercritical filaments. This supports the hypothesis that filamentary structures act as pathways for the accumulation of gas and dust, leading to core formation.<sup id="cite_ref-arxiv_66-0" class="reference"><a href="#cite_note-arxiv-66"><span class="cite-bracket">[</span>66<span class="cite-bracket">]</span></a></sup> </p> <figure class="mw-halign-center" typeof="mw:File/Thumb"><a href="/wiki/File:Filamentary_network_of_the_California_GMC_imaged_by_Herschel.png" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/en/thumb/3/37/Filamentary_network_of_the_California_GMC_imaged_by_Herschel.png/800px-Filamentary_network_of_the_California_GMC_imaged_by_Herschel.png" decoding="async" width="800" height="285" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/3/37/Filamentary_network_of_the_California_GMC_imaged_by_Herschel.png/1200px-Filamentary_network_of_the_California_GMC_imaged_by_Herschel.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/3/37/Filamentary_network_of_the_California_GMC_imaged_by_Herschel.png/1600px-Filamentary_network_of_the_California_GMC_imaged_by_Herschel.png 2x" data-file-width="1972" data-file-height="702" /></a><figcaption>Filamentary network of the California GMC imaged by Herschel.<sup id="cite_ref-arxiv_66-1" class="reference"><a href="#cite_note-arxiv-66"><span class="cite-bracket">[</span>66<span class="cite-bracket">]</span></a></sup></figcaption></figure> <p>Both the core mass function (CMF) and filament line mass function (FLMF) observed in the California GMC follow power-law distributions at the high-mass end, consistent with the Salpeter initial mass function (IMF). Current results strongly support the existence of a connection between the FLMF and the CMF/IMF, demonstrating that this connection holds at the level of an individual cloud, specifically the California GMC.<sup id="cite_ref-arxiv_66-2" class="reference"><a href="#cite_note-arxiv-66"><span class="cite-bracket">[</span>66<span class="cite-bracket">]</span></a></sup> The FLMF presented is a distribution of local line masses for a complete, homogeneous sample of filaments within the same cloud. It is the local line mass of a filament that defines its ability to fragment at a particular location along its spine, not the average line mass of the filament. This connection is more direct and provides tighter constraints on the origin of the CMF/IMF.<sup id="cite_ref-arxiv_66-3" class="reference"><a href="#cite_note-arxiv-66"><span class="cite-bracket">[</span>66<span class="cite-bracket">]</span></a></sup> </p> <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=Star_formation&action=edit&section=10" title="Edit section: See also"><span>edit</span></a><span class="mw-editsection-bracket">]</span></span></div> <ul><li><a href="/wiki/Accretion_(astrophysics)" title="Accretion (astrophysics)">Accretion</a> – Accumulation of particles into a massive object by gravitationally attracting more matter</li> <li><a href="/wiki/Champagne_flow_model" title="Champagne flow model">Champagne flow model</a></li> <li><a href="/wiki/Chronology_of_the_universe" title="Chronology of the universe">Chronology of the universe</a> – History and future of the universe</li> <li><a href="/wiki/Formation_and_evolution_of_the_Solar_System" title="Formation and evolution of the Solar System">Formation and evolution of the Solar System</a></li> <li><a href="/wiki/Galaxy_formation_and_evolution" title="Galaxy formation and evolution">Galaxy formation and evolution</a></li> <li><a href="/wiki/List_of_star-forming_regions_in_the_Local_Group" title="List of star-forming regions in the Local Group">List of star-forming regions in the Local Group</a> – Regions in the Milky Way galaxy and Local Group where new stars are forming</li> <li><a href="/wiki/Pea_galaxy" title="Pea galaxy">Pea galaxy</a> – Possible type of luminous blue compact galaxy</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=Star_formation&action=edit&section=11" 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 .reflist-lower-roman{list-style-type:lower-roman}</style><div class="reflist reflist-columns references-column-width" style="column-width: 30em;"> <ol class="references"> <li id="cite_note-1"><span class="mw-cite-backlink"><b><a href="#cite_ref-1">^</a></b></span> <span class="reference-text"><style data-mw-deduplicate="TemplateStyles:r1238218222">.mw-parser-output cite.citation{font-style:inherit;word-wrap:break-word}.mw-parser-output .citation q{quotes:"\"""\"""'""'"}.mw-parser-output .citation:target{background-color:rgba(0,127,255,0.133)}.mw-parser-output .id-lock-free.id-lock-free a{background:url("//upload.wikimedia.org/wikipedia/commons/6/65/Lock-green.svg")right 0.1em center/9px no-repeat}.mw-parser-output .id-lock-limited.id-lock-limited a,.mw-parser-output .id-lock-registration.id-lock-registration a{background:url("//upload.wikimedia.org/wikipedia/commons/d/d6/Lock-gray-alt-2.svg")right 0.1em center/9px no-repeat}.mw-parser-output .id-lock-subscription.id-lock-subscription a{background:url("//upload.wikimedia.org/wikipedia/commons/a/aa/Lock-red-alt-2.svg")right 0.1em center/9px no-repeat}.mw-parser-output .cs1-ws-icon a{background:url("//upload.wikimedia.org/wikipedia/commons/4/4c/Wikisource-logo.svg")right 0.1em center/12px no-repeat}body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .id-lock-free a,body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .id-lock-limited a,body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .id-lock-registration a,body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .id-lock-subscription a,body:not(.skin-timeless):not(.skin-minerva) .mw-parser-output .cs1-ws-icon a{background-size:contain;padding:0 1em 0 0}.mw-parser-output .cs1-code{color:inherit;background:inherit;border:none;padding:inherit}.mw-parser-output .cs1-hidden-error{display:none;color:var(--color-error,#d33)}.mw-parser-output .cs1-visible-error{color:var(--color-error,#d33)}.mw-parser-output .cs1-maint{display:none;color:#085;margin-left:0.3em}.mw-parser-output .cs1-kern-left{padding-left:0.2em}.mw-parser-output .cs1-kern-right{padding-right:0.2em}.mw-parser-output .citation .mw-selflink{font-weight:inherit}@media screen{.mw-parser-output .cs1-format{font-size:95%}html.skin-theme-clientpref-night .mw-parser-output .cs1-maint{color:#18911f}}@media screen and (prefers-color-scheme:dark){html.skin-theme-clientpref-os .mw-parser-output .cs1-maint{color:#18911f}}</style><cite id="CITEREFStahler,_S._W.Palla,_F.2004" class="citation book cs1">Stahler, S. 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href="/wiki/Template:Star" title="Template:Star"><abbr title="View this template">v</abbr></a></li><li class="nv-talk"><a href="/wiki/Template_talk:Star" title="Template talk:Star"><abbr title="Discuss this template">t</abbr></a></li><li class="nv-edit"><a href="/wiki/Special:EditPage/Template:Star" title="Special:EditPage/Template:Star"><abbr title="Edit this template">e</abbr></a></li></ul></div><div id="Stars" style="font-size:114%;margin:0 4em"><a href="/wiki/Star" title="Star">Stars</a></div></th></tr><tr><td class="navbox-abovebelow" colspan="2"><div> <ul><li><a href="/wiki/Lists_of_stars" title="Lists of stars">List</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a class="mw-selflink selflink">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 href="/wiki/Stellar_kinematics" title="Stellar kinematics">Kinematics</a></li> <li><a href="/wiki/Stellar_magnetic_field" title="Stellar magnetic field">Magnetic field</a></li> <li><a href="/wiki/Absolute_magnitude" title="Absolute magnitude">Absolute magnitude</a></li> <li><a href="/wiki/Stellar_mass" title="Stellar mass">Mass</a></li> <li><a href="/wiki/Metallicity" title="Metallicity">Metallicity</a></li> <li><a href="/wiki/Stellar_rotation" title="Stellar rotation">Rotation</a></li> <li><a href="/wiki/Starlight" title="Starlight">Starlight</a></li> <li><a href="/wiki/Variable_star" title="Variable star">Variable</a></li> <li><a href="/wiki/Photometric_system" title="Photometric system">Photometric system</a></li> <li><a href="/wiki/Color_index" title="Color index">Color index</a></li> <li><a href="/wiki/Hertzsprung%E2%80%93Russell_diagram" title="Hertzsprung–Russell diagram">Hertzsprung–Russell diagram</a></li> <li><a href="/wiki/Color%E2%80%93color_diagram" title="Color–color diagram">Color–color diagram</a></li> <li><a href="/wiki/Str%C3%B6mgren_sphere" title="Strömgren sphere">Strömgren sphere</a></li> <li><a href="/wiki/Kraft_break" title="Kraft break">Kraft break</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Star_system" title="Star system">Star systems</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Binary_star" title="Binary star">Binary</a> <ul><li><a href="/wiki/Contact_binary" title="Contact binary">Contact</a></li> <li><a href="/wiki/Common_envelope" title="Common envelope">Common envelope</a></li> <li><a href="/wiki/Eclipsing_binary" class="mw-redirect" title="Eclipsing binary">Eclipsing</a></li> <li><a href="/wiki/Symbiotic_binary" title="Symbiotic binary">Symbiotic</a></li></ul></li> <li><a href="/wiki/Star_system#Multiple_star_systems" title="Star system">Multiple</a></li> <li><a href="/wiki/Star_cluster" title="Star cluster">Cluster</a> <ul><li><a href="/wiki/Open_cluster" title="Open cluster">Open</a></li> <li><a href="/wiki/Globular_cluster" title="Globular cluster">Globular</a></li> <li><a href="/wiki/Super_star_cluster" title="Super star cluster">Super</a></li></ul></li> <li><a href="/wiki/Planetary_system" title="Planetary system">Planetary system</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Earth-centric<br />observations</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Sun" title="Sun">Sun</a> <ul><li><a href="/wiki/Solar_eclipse" title="Solar eclipse">Solar eclipse</a></li> <li><a href="/wiki/Solar_radio_emission" title="Solar radio emission">Solar radio emission</a></li> <li><a href="/wiki/Solar_System" title="Solar System">Solar System</a></li> <li><a href="/wiki/Sunlight" title="Sunlight">Sunlight</a></li></ul></li> <li><a href="/wiki/Pole_star" title="Pole star">Pole star</a></li> <li><a href="/wiki/Circumpolar_star" title="Circumpolar star">Circumpolar</a></li> <li><a href="/wiki/Constellation" title="Constellation">Constellation</a></li> <li><a href="/wiki/Asterism_(astronomy)" title="Asterism (astronomy)">Asterism</a></li> <li><a href="/wiki/Magnitude_(astronomy)" title="Magnitude (astronomy)">Magnitude</a> <ul><li><a href="/wiki/Apparent_magnitude" title="Apparent magnitude">Apparent</a></li> <li><a href="/wiki/Extinction_(astronomy)" title="Extinction (astronomy)">Extinction</a></li> <li><a href="/wiki/Photographic_magnitude" title="Photographic magnitude">Photographic</a></li></ul></li> <li><a href="/wiki/Radial_velocity" title="Radial velocity">Radial velocity</a></li> <li><a href="/wiki/Proper_motion" title="Proper motion">Proper motion</a></li> <li><a href="/wiki/Stellar_parallax" title="Stellar parallax">Parallax</a></li> <li><a href="/wiki/Photometric-standard_star" title="Photometric-standard star">Photometric-standard</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Lists_of_stars" title="Lists of stars">Lists</a></th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/List_of_proper_names_of_stars" title="List of proper names of stars">Proper names</a> <ul><li><a href="/wiki/List_of_Arabic_star_names" title="List of Arabic star names">Arabic</a></li> <li><a href="/wiki/Chinese_star_names" class="mw-redirect" title="Chinese star names">Chinese</a></li></ul></li> <li><a href="/wiki/List_of_star_extremes" title="List of star extremes">Extremes</a> <ul><li><a href="/wiki/List_of_most_massive_stars" title="List of most massive stars">Most massive</a></li> <li><a href="/wiki/List_of_hottest_stars" title="List of hottest stars">Highest temperature</a></li> <li><a href="/wiki/List_of_coolest_stars" title="List of coolest stars">Lowest temperature</a></li> <li><a href="/wiki/List_of_largest_known_stars" class="mw-redirect" title="List of largest known stars">Largest volume</a></li> <li><a href="/wiki/List_of_smallest_known_stars" title="List of smallest known stars">Smallest volume</a></li> <li><a href="/wiki/List_of_brightest_stars" title="List of brightest stars">Brightest</a></li> <li><a href="/wiki/Historical_brightest_stars" title="Historical brightest stars">Historical brightest</a></li> <li><a href="/wiki/List_of_most_luminous_stars" title="List of most luminous stars">Most luminous</a></li> <li><a href="/wiki/List_of_nearest_stars" title="List of nearest stars">Nearest</a> <ul><li><a href="/wiki/List_of_nearest_bright_stars" title="List of nearest bright stars">bright</a></li></ul></li> <li><a href="/wiki/List_of_the_most_distant_astronomical_objects#List_of_most_distant_objects_by_type" title="List of the most distant astronomical objects">Most distant</a></li></ul></li> <li><a href="/wiki/List_of_stars_with_resolved_images" title="List of stars with resolved images">With resolved images</a></li> <li><a href="/wiki/List_of_multiplanetary_systems" title="List of multiplanetary systems">With multiple exoplanets</a></li> <li><a href="/wiki/List_of_brown_dwarfs" title="List of brown dwarfs">Brown dwarfs</a></li> <li><a href="/wiki/List_of_red_dwarfs" title="List of red dwarfs">Red dwarfs</a></li> <li><a href="/wiki/List_of_white_dwarfs" title="List of white dwarfs">White dwarfs</a></li> <li><a href="/wiki/List_of_novae_in_the_Milky_Way_galaxy" title="List of novae in the Milky Way galaxy">Milky Way novae</a></li> <li><a href="/wiki/List_of_supernovae" title="List of supernovae">Supernovae</a> <ul><li><a href="/wiki/List_of_supernova_candidates" title="List of supernova candidates">Candidates</a></li> <li><a href="/wiki/List_of_supernova_remnants" title="List of supernova remnants">Remnants</a></li></ul></li> <li><a href="/wiki/List_of_planetary_nebulae" title="List of planetary nebulae">Planetary nebulae</a></li> <li><a href="/wiki/Timeline_of_stellar_astronomy" title="Timeline of stellar astronomy">Timeline of stellar astronomy</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Related</th><td class="navbox-list-with-group navbox-list navbox-even" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Substellar_object" title="Substellar object">Substellar object</a> <ul><li><a href="/wiki/Brown_dwarf" title="Brown dwarf">Brown dwarf</a> <ul><li><a href="/wiki/Brown-dwarf_desert" title="Brown-dwarf desert">Desert</a></li> <li><a href="/wiki/Sub-brown_dwarf" title="Sub-brown dwarf">Sub</a></li></ul></li> <li><a href="/wiki/Planet" title="Planet">Planet</a></li></ul></li> <li><a href="/wiki/Galactic_year" title="Galactic year">Galactic year</a></li> <li><a href="/wiki/Galaxy" title="Galaxy">Galaxy</a></li> <li><a href="/wiki/Guest_star_(astronomy)" title="Guest star (astronomy)">Guest</a></li> <li><a href="/wiki/Gravity" title="Gravity">Gravity</a></li> <li><a href="/wiki/Intergalactic_star" title="Intergalactic star">Intergalactic</a></li> <li><a href="/wiki/Planet-hosting_stars" class="mw-redirect" title="Planet-hosting stars">Planet-hosting stars</a></li> <li><a href="/wiki/Tidal_disruption_event" title="Tidal disruption event">Tidal disruption event</a></li></ul> </div></td></tr><tr><td class="navbox-abovebelow" colspan="2"><div> <ul><li><span class="noviewer" typeof="mw:File"><span title="Category"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/16px-Symbol_category_class.svg.png" decoding="async" width="16" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/23px-Symbol_category_class.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/31px-Symbol_category_class.svg.png 2x" data-file-width="180" data-file-height="185" /></span></span> <a href="/wiki/Category:Stars" title="Category:Stars">Category</a></li> <li><span class="nowrap"><span class="noviewer" typeof="mw:File"><a href="/wiki/File:He1523a.jpg" class="mw-file-description"><img alt="icon" src="//upload.wikimedia.org/wikipedia/commons/thumb/5/5f/He1523a.jpg/14px-He1523a.jpg" decoding="async" width="14" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/5/5f/He1523a.jpg/21px-He1523a.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/5/5f/He1523a.jpg/28px-He1523a.jpg 2x" data-file-width="180" data-file-height="207" /></a></span> </span><a href="/wiki/Portal:Stars" title="Portal:Stars">Stars portal</a></li></ul> </div></td></tr></tbody></table></div> <div class="navbox-styles"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1129693374"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1236075235"></div><div role="navigation" class="navbox" aria-labelledby="Star_formation" style="padding:3px"><table class="nowraplinks hlist mw-collapsible autocollapse navbox-inner" style="border-spacing:0;background:transparent;color:inherit"><tbody><tr><th scope="col" class="navbox-title" colspan="3" style="text-align: center;"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1129693374"><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1239400231"><div class="navbar plainlinks hlist navbar-mini"><ul><li class="nv-view"><a href="/wiki/Template:Star_formation_navbox" title="Template:Star formation navbox"><abbr title="View this template">v</abbr></a></li><li class="nv-talk"><a href="/wiki/Template_talk:Star_formation_navbox" title="Template talk:Star formation navbox"><abbr title="Discuss this template">t</abbr></a></li><li class="nv-edit"><a href="/wiki/Special:EditPage/Template:Star_formation_navbox" title="Special:EditPage/Template:Star formation navbox"><abbr title="Edit this template">e</abbr></a></li></ul></div><div id="Star_formation" style="font-size:114%;margin:0 4em"><a class="mw-selflink selflink">Star formation</a></div></th></tr><tr><th scope="row" class="navbox-group" style="text-align: center;;width:1%">Object classes</th><td class="navbox-list-with-group navbox-list navbox-odd" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Interstellar_medium" title="Interstellar medium">Interstellar medium</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/Dark_nebula" title="Dark nebula">Dark nebula</a></li> <li><a href="/wiki/Young_stellar_object" title="Young stellar object">Young stellar object</a></li> <li><a href="/wiki/Protostar" title="Protostar">Protostar</a></li> <li><a href="/wiki/T_Tauri_star" title="T Tauri star">T Tauri star</a></li> <li><a href="/wiki/Pre-main-sequence_star" title="Pre-main-sequence star">Pre-main-sequence star</a></li> <li><a href="/wiki/Herbig_Ae/Be_star" title="Herbig Ae/Be star">Herbig Ae/Be star</a></li> <li><a href="/wiki/Herbig%E2%80%93Haro_object" title="Herbig–Haro object">Herbig–Haro object</a></li></ul> </div></td><td class="noviewer navbox-image" rowspan="2" style="width:1px;padding:0 0 0 2px"><div><span typeof="mw:File"><span><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/8/87/LH_95.jpg/80px-LH_95.jpg" decoding="async" width="80" height="86" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/8/87/LH_95.jpg/120px-LH_95.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/8/87/LH_95.jpg/160px-LH_95.jpg 2x" data-file-width="3622" data-file-height="3877" /></span></span></div></td></tr><tr><th scope="row" class="navbox-group" style="text-align: center;;width:1%">Theoretical concepts</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/Initial_mass_function" title="Initial mass function">Initial mass function</a></li> <li><a href="/wiki/Jeans_instability" title="Jeans instability">Jeans instability</a></li> <li><a href="/wiki/Kelvin%E2%80%93Helmholtz_mechanism" title="Kelvin–Helmholtz mechanism">Kelvin–Helmholtz mechanism</a></li> <li><a href="/wiki/Nebular_hypothesis" title="Nebular hypothesis">Nebular hypothesis</a></li> <li><a href="/wiki/Planetary_migration" title="Planetary migration">Planetary migration</a></li></ul> </div></td></tr><tr><td class="navbox-abovebelow" colspan="3" style="text-align: center;"><div> <ul><li><span class="noviewer" typeof="mw:File"><span title="Category"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/16px-Symbol_category_class.svg.png" decoding="async" width="16" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/23px-Symbol_category_class.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/9/96/Symbol_category_class.svg/31px-Symbol_category_class.svg.png 2x" data-file-width="180" data-file-height="185" /></span></span> <a href="/wiki/Category:Star_formation" title="Category:Star formation"><b>Category</b></a></li> <li><span class="noviewer" typeof="mw:File"><a href="/wiki/File:Symbol_portal_class.svg" class="mw-file-description" title="Portal"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/e/e2/Symbol_portal_class.svg/16px-Symbol_portal_class.svg.png" decoding="async" width="16" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/e/e2/Symbol_portal_class.svg/23px-Symbol_portal_class.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/e/e2/Symbol_portal_class.svg/31px-Symbol_portal_class.svg.png 2x" data-file-width="180" data-file-height="185" /></a></span> <a href="/wiki/Portal:Stars" title="Portal:Stars"><b>Stars portal</b></a></li> <li><span class="noviewer" typeof="mw:File"><span title="Commons page"><img alt="" src="//upload.wikimedia.org/wikipedia/en/thumb/4/4a/Commons-logo.svg/12px-Commons-logo.svg.png" decoding="async" width="12" height="16" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/en/thumb/4/4a/Commons-logo.svg/18px-Commons-logo.svg.png 1.5x, //upload.wikimedia.org/wikipedia/en/thumb/4/4a/Commons-logo.svg/24px-Commons-logo.svg.png 2x" data-file-width="1024" data-file-height="1376" /></span></span> <a href="https://commons.wikimedia.org/wiki/Category:Star_formation" class="extiw" title="commons:Category:Star formation"><b>Commons</b></a></li></ul> </div></td></tr></tbody></table></div> <style data-mw-deduplicate="TemplateStyles:r1130092004">.mw-parser-output .portal-bar{font-size:88%;font-weight:bold;display:flex;justify-content:center;align-items:baseline}.mw-parser-output .portal-bar-bordered{padding:0 2em;background-color:#fdfdfd;border:1px solid #a2a9b1;clear:both;margin:1em auto 0}.mw-parser-output .portal-bar-related{font-size:100%;justify-content:flex-start}.mw-parser-output .portal-bar-unbordered{padding:0 1.7em;margin-left:0}.mw-parser-output .portal-bar-header{margin:0 1em 0 0.5em;flex:0 0 auto;min-height:24px}.mw-parser-output .portal-bar-content{display:flex;flex-flow:row wrap;flex:0 1 auto;padding:0.15em 0;column-gap:1em;align-items:baseline;margin:0;list-style:none}.mw-parser-output .portal-bar-content-related{margin:0;list-style:none}.mw-parser-output .portal-bar-item{display:inline-block;margin:0.15em 0.2em;min-height:24px;line-height:24px}@media screen and (max-width:768px){.mw-parser-output .portal-bar{font-size:88%;font-weight:bold;display:flex;flex-flow:column wrap;align-items:baseline}.mw-parser-output .portal-bar-header{text-align:center;flex:0;padding-left:0.5em;margin:0 auto}.mw-parser-output .portal-bar-related{font-size:100%;align-items:flex-start}.mw-parser-output .portal-bar-content{display:flex;flex-flow:row wrap;align-items:center;flex:0;column-gap:1em;border-top:1px solid #a2a9b1;margin:0 auto;list-style:none}.mw-parser-output .portal-bar-content-related{border-top:none;margin:0;list-style:none}}.mw-parser-output .navbox+link+.portal-bar,.mw-parser-output .navbox+style+.portal-bar,.mw-parser-output .navbox+link+.portal-bar-bordered,.mw-parser-output .navbox+style+.portal-bar-bordered,.mw-parser-output .sister-bar+link+.portal-bar,.mw-parser-output .sister-bar+style+.portal-bar,.mw-parser-output .portal-bar+.navbox-styles+.navbox,.mw-parser-output .portal-bar+.navbox-styles+.sister-bar{margin-top:-1px}</style><div class="portal-bar noprint metadata noviewer portal-bar-bordered" role="navigation" aria-label="Portals"><span class="portal-bar-header"><a href="/wiki/Wikipedia:Contents/Portals" title="Wikipedia:Contents/Portals">Portals</a>:</span><ul class="portal-bar-content"><li class="portal-bar-item"><span class="nowrap"><span typeof="mw:File"><span><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/0/00/Crab_Nebula.jpg/19px-Crab_Nebula.jpg" decoding="async" width="19" height="19" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/0/00/Crab_Nebula.jpg/29px-Crab_Nebula.jpg 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/0/00/Crab_Nebula.jpg/38px-Crab_Nebula.jpg 2x" data-file-width="3864" data-file-height="3864" /></span></span> </span><a href="/wiki/Portal:Astronomy" title="Portal:Astronomy">Astronomy</a></li><li class="portal-bar-item"><span class="nowrap"><span typeof="mw:File"><span><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/d/d6/RocketSunIcon.svg/19px-RocketSunIcon.svg.png" decoding="async" width="19" height="19" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/d/d6/RocketSunIcon.svg/29px-RocketSunIcon.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/d/d6/RocketSunIcon.svg/38px-RocketSunIcon.svg.png 2x" data-file-width="128" data-file-height="128" /></span></span> </span><a href="/wiki/Portal:Spaceflight" title="Portal:Spaceflight">Spaceflight</a></li><li class="portal-bar-item"><span class="nowrap"><span typeof="mw:File"><span><img alt="" src="//upload.wikimedia.org/wikipedia/commons/thumb/5/5c/Earth-moon.jpg/21px-Earth-moon.jpg" decoding="async" width="21" height="17" class="mw-file-element" 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