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class="vector-toc-list"> </ul> </li> <li id="toc-CNO-II" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#CNO-II"> <div class="vector-toc-text"> 1.2 CNO-II </div> </a> <ul id="toc-CNO-II-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-CNO-III" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#CNO-III"> <div class="vector-toc-text"> 1.3 CNO-III </div> </a> <ul id="toc-CNO-III-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-CNO-IV" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#CNO-IV"> <div class="vector-toc-text"> 1.4 CNO-IV </div> </a> <ul id="toc-CNO-IV-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Hot_CNO_cycles" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#Hot_CNO_cycles"> <div class="vector-toc-text"> 2 Hot CNO cycles </div> </a> <button aria-controls="toc-Hot_CNO_cycles-sublist" class="cdx-button cdx-button--weight-quiet cdx-button--icon-only vector-toc-toggle"> Toggle Hot CNO cycles subsection </button> <ul id="toc-Hot_CNO_cycles-sublist" class="vector-toc-list"> <li id="toc-HCNO-I" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#HCNO-I"> <div class="vector-toc-text"> 2.1 HCNO-I </div> </a> <ul id="toc-HCNO-I-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-HCNO-II" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#HCNO-II"> <div class="vector-toc-text"> 2.2 HCNO-II </div> </a> <ul id="toc-HCNO-II-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-HCNO-III" class="vector-toc-list-item vector-toc-level-2"> <a class="vector-toc-link" href="#HCNO-III"> <div class="vector-toc-text"> 2.3 HCNO-III </div> </a> <ul id="toc-HCNO-III-sublist" class="vector-toc-list"> </ul> </li> </ul> </li> <li id="toc-Use_in_astronomy" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#Use_in_astronomy"> <div class="vector-toc-text"> 3 Use in astronomy </div> </a> <ul id="toc-Use_in_astronomy-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"> 4 See also </div> </a> <ul id="toc-See_also-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Footnotes" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#Footnotes"> <div class="vector-toc-text"> 5 Footnotes </div> </a> <ul id="toc-Footnotes-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"> 6 References </div> </a> <ul id="toc-References-sublist" class="vector-toc-list"> </ul> </li> <li id="toc-Further_reading" class="vector-toc-list-item vector-toc-level-1 vector-toc-list-item-expanded"> <a class="vector-toc-link" href="#Further_reading"> <div class="vector-toc-text"> 7 Further reading </div> </a> <ul id="toc-Further_reading-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" > Toggle the table of contents </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">CNO cycle</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 43 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-43" aria-hidden="true" > 43 languages </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/CNO-siklus" title="CNO-siklus – Afrikaans" lang="af" hreflang="af" data-title="CNO-siklus" data-language-autonym="Afrikaans" data-language-local-name="Afrikaans" class="interlanguage-link-target">Afrikaans</a></li><li class="interlanguage-link interwiki-ar mw-list-item"><a href="https://ar.wikipedia.org/wiki/%D8%AF%D9%88%D8%B1%D8%A9_%D9%83%D8%B1%D8%A8%D9%88%D9%86-%D9%86%D9%8A%D8%AA%D8%B1%D9%88%D8%AC%D9%8A%D9%86-%D8%A3%D9%83%D8%B3%D8%AC%D9%8A%D9%86" title="دورة كربون-نيتروجين-أكسجين – Arabic" lang="ar" hreflang="ar" data-title="دورة كربون-نيتروجين-أكسجين" data-language-autonym="العربية" data-language-local-name="Arabic" class="interlanguage-link-target">العربية</a></li><li class="interlanguage-link interwiki-bn mw-list-item"><a href="https://bn.wikipedia.org/wiki/%E0%A6%95%E0%A6%BE%E0%A6%B0%E0%A7%8D%E0%A6%AC%E0%A6%A8-%E0%A6%A8%E0%A6%BE%E0%A6%87%E0%A6%9F%E0%A7%8D%E0%A6%B0%E0%A7%8B%E0%A6%9C%E0%A7%87%E0%A6%A8-%E0%A6%85%E0%A6%95%E0%A7%8D%E0%A6%B8%E0%A6%BF%E0%A6%9C%E0%A7%87%E0%A6%A8_%E0%A6%9A%E0%A6%95%E0%A7%8D%E0%A6%B0" title="কার্বন-নাইট্রোজেন-অক্সিজেন চক্র – Bangla" lang="bn" hreflang="bn" data-title="কার্বন-নাইট্রোজেন-অক্সিজেন চক্র" data-language-autonym="বাংলা" data-language-local-name="Bangla" class="interlanguage-link-target">বাংলা</a></li><li class="interlanguage-link interwiki-ca mw-list-item"><a href="https://ca.wikipedia.org/wiki/Cicle_CNO" title="Cicle CNO – Catalan" lang="ca" hreflang="ca" data-title="Cicle CNO" data-language-autonym="Català" data-language-local-name="Catalan" class="interlanguage-link-target">Català</a></li><li class="interlanguage-link interwiki-cs mw-list-item"><a href="https://cs.wikipedia.org/wiki/CNO_cyklus" title="CNO cyklus – Czech" lang="cs" hreflang="cs" data-title="CNO cyklus" data-language-autonym="Čeština" data-language-local-name="Czech" class="interlanguage-link-target">Čeština</a></li><li class="interlanguage-link interwiki-da mw-list-item"><a href="https://da.wikipedia.org/wiki/CNO-cyklus" title="CNO-cyklus – Danish" lang="da" hreflang="da" data-title="CNO-cyklus" data-language-autonym="Dansk" data-language-local-name="Danish" class="interlanguage-link-target">Dansk</a></li><li class="interlanguage-link interwiki-de mw-list-item"><a href="https://de.wikipedia.org/wiki/Bethe-Weizs%C3%A4cker-Zyklus" title="Bethe-Weizsäcker-Zyklus – German" lang="de" hreflang="de" data-title="Bethe-Weizsäcker-Zyklus" data-language-autonym="Deutsch" data-language-local-name="German" class="interlanguage-link-target">Deutsch</a></li><li class="interlanguage-link interwiki-et mw-list-item"><a href="https://et.wikipedia.org/wiki/Bethe_ts%C3%BCkkel" title="Bethe tsükkel – Estonian" lang="et" hreflang="et" data-title="Bethe tsükkel" data-language-autonym="Eesti" data-language-local-name="Estonian" class="interlanguage-link-target">Eesti</a></li><li class="interlanguage-link interwiki-el mw-list-item"><a href="https://el.wikipedia.org/wiki/%CE%9A%CF%8D%CE%BA%CE%BB%CE%BF%CF%82_CNO" title="Κύκλος CNO – Greek" lang="el" hreflang="el" data-title="Κύκλος CNO" data-language-autonym="Ελληνικά" data-language-local-name="Greek" class="interlanguage-link-target">Ελληνικά</a></li><li class="interlanguage-link interwiki-es mw-list-item"><a href="https://es.wikipedia.org/wiki/Ciclo_CNO" title="Ciclo CNO – Spanish" lang="es" hreflang="es" data-title="Ciclo CNO" data-language-autonym="Español" data-language-local-name="Spanish" class="interlanguage-link-target">Español</a></li><li class="interlanguage-link interwiki-fa mw-list-item"><a href="https://fa.wikipedia.org/wiki/%DA%86%D8%B1%D8%AE%D9%87_%D8%B3%DB%8C%E2%80%8C%D8%A7%D9%86%E2%80%8C%D8%A7%D9%88" title="چرخه سی‌ان‌او – Persian" lang="fa" hreflang="fa" data-title="چرخه سی‌ان‌او" data-language-autonym="فارسی" data-language-local-name="Persian" class="interlanguage-link-target">فارسی</a></li><li class="interlanguage-link interwiki-fr mw-list-item"><a href="https://fr.wikipedia.org/wiki/Cycle_carbone-azote-oxyg%C3%A8ne" title="Cycle carbone-azote-oxygène – French" lang="fr" hreflang="fr" data-title="Cycle carbone-azote-oxygène" data-language-autonym="Français" data-language-local-name="French" class="interlanguage-link-target">Français</a></li><li class="interlanguage-link interwiki-gl mw-list-item"><a href="https://gl.wikipedia.org/wiki/Ciclo_carbono-nitr%C3%B3xeno-os%C3%ADxeno" title="Ciclo carbono-nitróxeno-osíxeno – Galician" lang="gl" hreflang="gl" data-title="Ciclo carbono-nitróxeno-osíxeno" data-language-autonym="Galego" data-language-local-name="Galician" class="interlanguage-link-target">Galego</a></li><li class="interlanguage-link interwiki-ko mw-list-item"><a href="https://ko.wikipedia.org/wiki/CNO_%EC%88%9C%ED%99%98" title="CNO 순환 – Korean" lang="ko" hreflang="ko" data-title="CNO 순환" data-language-autonym="한국어" data-language-local-name="Korean" class="interlanguage-link-target">한국어</a></li><li class="interlanguage-link interwiki-hr mw-list-item"><a href="https://hr.wikipedia.org/wiki/Niz_ugljik-du%C5%A1ik-kisik" title="Niz ugljik-dušik-kisik – Croatian" lang="hr" hreflang="hr" data-title="Niz ugljik-dušik-kisik" data-language-autonym="Hrvatski" data-language-local-name="Croatian" class="interlanguage-link-target">Hrvatski</a></li><li class="interlanguage-link interwiki-id mw-list-item"><a href="https://id.wikipedia.org/wiki/Siklus_CNO" title="Siklus CNO – Indonesian" lang="id" hreflang="id" data-title="Siklus CNO" data-language-autonym="Bahasa Indonesia" data-language-local-name="Indonesian" class="interlanguage-link-target">Bahasa Indonesia</a></li><li class="interlanguage-link interwiki-it mw-list-item"><a href="https://it.wikipedia.org/wiki/Ciclo_del_carbonio-azoto-ossigeno" title="Ciclo del carbonio-azoto-ossigeno – Italian" lang="it" hreflang="it" data-title="Ciclo del carbonio-azoto-ossigeno" data-language-autonym="Italiano" data-language-local-name="Italian" class="interlanguage-link-target">Italiano</a></li><li class="interlanguage-link interwiki-he mw-list-item"><a href="https://he.wikipedia.org/wiki/%D7%9E%D7%97%D7%96%D7%95%D7%A8_CNO" title="מחזור CNO – Hebrew" lang="he" hreflang="he" data-title="מחזור CNO" data-language-autonym="עברית" data-language-local-name="Hebrew" class="interlanguage-link-target">עברית</a></li><li class="interlanguage-link interwiki-jv mw-list-item"><a href="https://jv.wikipedia.org/wiki/Siklus_CNO" title="Siklus CNO – Javanese" lang="jv" hreflang="jv" data-title="Siklus CNO" data-language-autonym="Jawa" data-language-local-name="Javanese" class="interlanguage-link-target">Jawa</a></li><li class="interlanguage-link interwiki-lt mw-list-item"><a href="https://lt.wikipedia.org/wiki/Anglies,_azoto_ir_deguonies_ciklas" title="Anglies, azoto ir deguonies ciklas – Lithuanian" lang="lt" hreflang="lt" data-title="Anglies, azoto ir deguonies ciklas" data-language-autonym="Lietuvių" data-language-local-name="Lithuanian" class="interlanguage-link-target">Lietuvių</a></li><li class="interlanguage-link interwiki-hu mw-list-item"><a href="https://hu.wikipedia.org/wiki/CNO-ciklus" title="CNO-ciklus – Hungarian" lang="hu" hreflang="hu" data-title="CNO-ciklus" data-language-autonym="Magyar" data-language-local-name="Hungarian" class="interlanguage-link-target">Magyar</a></li><li class="interlanguage-link interwiki-mk mw-list-item"><a href="https://mk.wikipedia.org/wiki/%D0%88%D0%B0%D0%B3%D0%BB%D0%B5%D1%80%D0%BE%D0%B4%D0%BD%D0%BE-%D0%B0%D0%B7%D0%BE%D1%82%D0%BD%D0%BE-%D0%BA%D0%B8%D1%81%D0%BB%D0%BE%D1%80%D0%BE%D0%B4%D0%B5%D0%BD_%D1%86%D0%B8%D0%BA%D0%BB%D1%83%D1%81" title="Јаглеродно-азотно-кислороден циклус – Macedonian" lang="mk" hreflang="mk" data-title="Јаглеродно-азотно-кислороден циклус" data-language-autonym="Македонски" data-language-local-name="Macedonian" class="interlanguage-link-target">Македонски</a></li><li class="interlanguage-link interwiki-ml mw-list-item"><a href="https://ml.wikipedia.org/wiki/%E0%B4%B8%E0%B4%BF.%E0%B4%8E%E0%B5%BB.%E0%B4%92._%E0%B4%9A%E0%B4%95%E0%B5%8D%E0%B4%B0%E0%B4%82" title="സി.എൻ.ഒ. ചക്രം – Malayalam" lang="ml" hreflang="ml" data-title="സി.എൻ.ഒ. ചക്രം" data-language-autonym="മലയാളം" data-language-local-name="Malayalam" class="interlanguage-link-target">മലയാളം</a></li><li class="interlanguage-link interwiki-ms mw-list-item"><a href="https://ms.wikipedia.org/wiki/Kitaran_CNO" title="Kitaran CNO – Malay" lang="ms" hreflang="ms" data-title="Kitaran CNO" data-language-autonym="Bahasa Melayu" data-language-local-name="Malay" class="interlanguage-link-target">Bahasa Melayu</a></li><li class="interlanguage-link interwiki-nl mw-list-item"><a href="https://nl.wikipedia.org/wiki/Koolstof-stikstofcyclus" title="Koolstof-stikstofcyclus – Dutch" lang="nl" hreflang="nl" data-title="Koolstof-stikstofcyclus" data-language-autonym="Nederlands" data-language-local-name="Dutch" class="interlanguage-link-target">Nederlands</a></li><li class="interlanguage-link interwiki-ja mw-list-item"><a href="https://ja.wikipedia.org/wiki/CNO%E3%82%B5%E3%82%A4%E3%82%AF%E3%83%AB" title="CNOサイクル – Japanese" lang="ja" hreflang="ja" data-title="CNOサイクル" data-language-autonym="日本語" data-language-local-name="Japanese" class="interlanguage-link-target">日本語</a></li><li class="interlanguage-link interwiki-no mw-list-item"><a href="https://no.wikipedia.org/wiki/CNO-syklusen" title="CNO-syklusen – Norwegian Bokmål" lang="nb" hreflang="nb" data-title="CNO-syklusen" data-language-autonym="Norsk bokmål" data-language-local-name="Norwegian Bokmål" class="interlanguage-link-target">Norsk bokmål</a></li><li class="interlanguage-link interwiki-nn mw-list-item"><a href="https://nn.wikipedia.org/wiki/CNO-syklusen" title="CNO-syklusen – Norwegian Nynorsk" lang="nn" hreflang="nn" data-title="CNO-syklusen" data-language-autonym="Norsk nynorsk" data-language-local-name="Norwegian Nynorsk" class="interlanguage-link-target">Norsk nynorsk</a></li><li class="interlanguage-link interwiki-pl mw-list-item"><a href="https://pl.wikipedia.org/wiki/Cykl_w%C4%99glowo-azotowo-tlenowy" title="Cykl węglowo-azotowo-tlenowy – Polish" lang="pl" hreflang="pl" data-title="Cykl węglowo-azotowo-tlenowy" data-language-autonym="Polski" data-language-local-name="Polish" class="interlanguage-link-target">Polski</a></li><li class="interlanguage-link interwiki-pt mw-list-item"><a href="https://pt.wikipedia.org/wiki/Ciclo_CNO" title="Ciclo CNO – Portuguese" lang="pt" hreflang="pt" data-title="Ciclo CNO" data-language-autonym="Português" data-language-local-name="Portuguese" class="interlanguage-link-target">Português</a></li><li class="interlanguage-link interwiki-ru mw-list-item"><a href="https://ru.wikipedia.org/wiki/CNO-%D1%86%D0%B8%D0%BA%D0%BB" title="CNO-цикл – Russian" lang="ru" hreflang="ru" data-title="CNO-цикл" data-language-autonym="Русский" data-language-local-name="Russian" class="interlanguage-link-target">Русский</a></li><li class="interlanguage-link interwiki-si mw-list-item"><a href="https://si.wikipedia.org/wiki/CNO_cycle" title="CNO cycle – Sinhala" lang="si" hreflang="si" data-title="CNO cycle" data-language-autonym="සිංහල" data-language-local-name="Sinhala" class="interlanguage-link-target">සිංහල</a></li><li class="interlanguage-link interwiki-sk mw-list-item"><a href="https://sk.wikipedia.org/wiki/Uhl%C3%ADkov%C3%BD_cyklus" title="Uhlíkový cyklus – Slovak" lang="sk" hreflang="sk" data-title="Uhlíkový cyklus" data-language-autonym="Slovenčina" data-language-local-name="Slovak" class="interlanguage-link-target">Slovenčina</a></li><li class="interlanguage-link interwiki-sr mw-list-item"><a href="https://sr.wikipedia.org/wiki/Niz_ugljenik-azot-kiseonik" title="Niz ugljenik-azot-kiseonik – Serbian" lang="sr" hreflang="sr" data-title="Niz ugljenik-azot-kiseonik" data-language-autonym="Српски / srpski" data-language-local-name="Serbian" class="interlanguage-link-target">Српски / srpski</a></li><li class="interlanguage-link interwiki-sh mw-list-item"><a href="https://sh.wikipedia.org/wiki/Niz_ugljik-du%C5%A1ik-kisik" title="Niz ugljik-dušik-kisik – Serbo-Croatian" lang="sh" hreflang="sh" data-title="Niz ugljik-dušik-kisik" data-language-autonym="Srpskohrvatski / српскохрватски" data-language-local-name="Serbo-Croatian" class="interlanguage-link-target">Srpskohrvatski / српскохрватски</a></li><li class="interlanguage-link interwiki-fi mw-list-item"><a href="https://fi.wikipedia.org/wiki/Hiilisykli" title="Hiilisykli – Finnish" lang="fi" hreflang="fi" data-title="Hiilisykli" data-language-autonym="Suomi" data-language-local-name="Finnish" class="interlanguage-link-target">Suomi</a></li><li class="interlanguage-link interwiki-sv mw-list-item"><a href="https://sv.wikipedia.org/wiki/CNO-cykeln" title="CNO-cykeln – Swedish" lang="sv" hreflang="sv" data-title="CNO-cykeln" data-language-autonym="Svenska" data-language-local-name="Swedish" class="interlanguage-link-target">Svenska</a></li><li class="interlanguage-link interwiki-ta mw-list-item"><a href="https://ta.wikipedia.org/wiki/%E0%AE%95%E0%AE%BE.%E0%AE%A8%E0%AF%88.%E0%AE%86_%E0%AE%9A%E0%AF%81%E0%AE%B4%E0%AE%B1%E0%AF%8D%E0%AE%9A%E0%AE%BF" title="கா.நை.ஆ சுழற்சி – Tamil" lang="ta" hreflang="ta" data-title="கா.நை.ஆ சுழற்சி" data-language-autonym="தமிழ்" data-language-local-name="Tamil" class="interlanguage-link-target">தமிழ்</a></li><li class="interlanguage-link interwiki-th mw-list-item"><a href="https://th.wikipedia.org/wiki/%E0%B8%A7%E0%B8%87%E0%B8%88%E0%B8%A3%E0%B8%8B%E0%B8%B5%E0%B9%80%E0%B8%AD%E0%B9%87%E0%B8%99%E0%B9%82%E0%B8%AD" title="วงจรซีเอ็นโอ – Thai" lang="th" hreflang="th" data-title="วงจรซีเอ็นโอ" data-language-autonym="ไทย" data-language-local-name="Thai" class="interlanguage-link-target">ไทย</a></li><li class="interlanguage-link interwiki-tr mw-list-item"><a href="https://tr.wikipedia.org/wiki/KAO_d%C3%B6ng%C3%BCs%C3%BC" title="KAO döngüsü – Turkish" lang="tr" hreflang="tr" data-title="KAO döngüsü" data-language-autonym="Türkçe" data-language-local-name="Turkish" class="interlanguage-link-target">Türkçe</a></li><li class="interlanguage-link interwiki-uk mw-list-item"><a href="https://uk.wikipedia.org/wiki/%D0%92%D1%83%D0%B3%D0%BB%D0%B5%D1%86%D0%B5%D0%B2%D0%BE-%D0%B0%D0%B7%D0%BE%D1%82%D0%BD%D0%B8%D0%B9_%D1%86%D0%B8%D0%BA%D0%BB" title="Вуглецево-азотний цикл – Ukrainian" lang="uk" hreflang="uk" data-title="Вуглецево-азотний цикл" data-language-autonym="Українська" data-language-local-name="Ukrainian" class="interlanguage-link-target">Українська</a></li><li class="interlanguage-link interwiki-vi mw-list-item"><a href="https://vi.wikipedia.org/wiki/Chu_tr%C3%ACnh_CNO" title="Chu trình CNO – Vietnamese" lang="vi" hreflang="vi" data-title="Chu trình CNO" data-language-autonym="Tiếng Việt" data-language-local-name="Vietnamese" class="interlanguage-link-target">Tiếng Việt</a></li><li class="interlanguage-link interwiki-zh mw-list-item"><a href="https://zh.wikipedia.org/wiki/%E7%A2%B3%E6%B0%AE%E6%B0%A7%E5%BE%AA%E7%92%B0" title="碳氮氧循環 – Chinese" lang="zh" hreflang="zh" data-title="碳氮氧循環" data-language-autonym="中文" data-language-local-name="Chinese" class="interlanguage-link-target">中文</a></li> </ul> <div class="after-portlet after-portlet-lang"><a href="https://www.wikidata.org/wiki/Special:EntityPage/Q222971#sitelinks-wikipedia" title="Edit interlanguage links" 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</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">Catalysed fusion reactions by which stars convert hydrogen to helium</div> <figure class="mw-halign-right" typeof="mw:File/Thumb"><a href="/wiki/File:Nuclear_energy_generation.svg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/5/5b/Nuclear_energy_generation.svg/300px-Nuclear_energy_generation.svg.png" decoding="async" width="300" height="245" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/5/5b/Nuclear_energy_generation.svg/450px-Nuclear_energy_generation.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/5/5b/Nuclear_energy_generation.svg/600px-Nuclear_energy_generation.svg.png 2x" data-file-width="642" data-file-height="525" /></a><figcaption><a href="/wiki/Logarithm" title="Logarithm">Logarithm</a> of the relative energy output (ε) of <a href="/wiki/Proton%E2%80%93proton_chain_reaction" class="mw-redirect" title="Proton–proton chain reaction">proton–proton</a> (p–p), CNO, and <a href="/wiki/Triple-alpha_process" title="Triple-alpha process">triple-α</a> fusion processes at different temperatures (T). The dashed line shows the combined energy generation of the p–p and CNO processes within a star.</figcaption></figure> The CNO cycle (for <a href="/wiki/Carbon" title="Carbon">carbon</a>–<a href="/wiki/Nitrogen" title="Nitrogen">nitrogen</a>–<a href="/wiki/Oxygen" title="Oxygen">oxygen</a>; sometimes called Bethe–Weizsäcker cycle after <a href="/wiki/Hans_Albrecht_Bethe" class="mw-redirect" title="Hans Albrecht Bethe">Hans Albrecht Bethe</a> and <a href="/wiki/Carl_Friedrich_von_Weizs%C3%A4cker" title="Carl Friedrich von Weizsäcker">Carl Friedrich von Weizsäcker</a>) is one of the two known sets of <a href="/wiki/Nuclear_fusion" title="Nuclear fusion">fusion</a> <a href="/wiki/Nuclear_reaction" title="Nuclear reaction">reactions</a> by which <a href="/wiki/Star" title="Star">stars</a> convert <a href="/wiki/Hydrogen" title="Hydrogen">hydrogen</a> to <a href="/wiki/Helium" title="Helium">helium</a>, the other being the <a href="/wiki/Proton%E2%80%93proton_chain_reaction" class="mw-redirect" title="Proton–proton chain reaction">proton–proton chain reaction</a> (p–p cycle), which is more efficient at the <a href="/wiki/Sun" title="Sun">Sun</a>'s core temperature. The CNO cycle is hypothesized to be dominant in stars that are more than 1.3 times as <a href="/wiki/Solar_mass" title="Solar mass">massive as the Sun</a>.<a href="#cite_note-salaris_cassini2005-1">[1]</a> Unlike the proton-proton reaction, which consumes all its constituents, the CNO cycle is a <a href="/wiki/Catalytic_cycle" title="Catalytic cycle">catalytic cycle</a>. In the CNO cycle, four <a href="/wiki/Proton" title="Proton">protons</a> fuse, using <a href="/wiki/Carbon" title="Carbon">carbon</a>, <a href="/wiki/Nitrogen" title="Nitrogen">nitrogen</a>, and <a href="/wiki/Oxygen" title="Oxygen">oxygen</a> isotopes as catalysts, each of which is consumed at one step of the CNO cycle, but re-generated in a later step. The end product is one <a href="/wiki/Alpha_particle" title="Alpha particle">alpha particle</a> (a <a href="/wiki/Stable_nuclide" title="Stable nuclide">stable</a> <a href="/wiki/Helium" title="Helium">helium</a> nucleus), two <a href="/wiki/Positron" title="Positron">positrons</a>, and two <a href="/wiki/Electron_neutrino" title="Electron neutrino">electron neutrinos</a>. There are various alternative paths and catalysts involved in the CNO cycles, but all these cycles have the same net result: <dl><dd>4 1 1H   +   2 e− <dl><dd>  →   4 2He   +   2 e+   +   2 e−   +   2 ν e   +   3 γ   +   24.7 <a href="/wiki/Electronvolt" title="Electronvolt">MeV</a></dd> <dd>  →   4 2He   +   2 ν e   +   7 γ   +   26.7 MeV</dd></dl></dd></dl> The positrons will almost instantly <a href="/wiki/Electron%E2%80%93positron_annihilation" title="Electron–positron annihilation">annihilate with electrons</a>, releasing energy in the form of <a href="/wiki/Gamma_ray" title="Gamma ray">gamma rays</a>. The neutrinos escape from the star carrying away some energy.<a href="#cite_note-BOREXINO-2">[2]</a> One nucleus goes on to become carbon, nitrogen, and oxygen isotopes through a number of transformations in a repeating cycle. <figure class="mw-halign-right" typeof="mw:File/Thumb"><a href="/wiki/File:CNO_Cycle.svg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/2/21/CNO_Cycle.svg/300px-CNO_Cycle.svg.png" decoding="async" width="300" height="300" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/2/21/CNO_Cycle.svg/450px-CNO_Cycle.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/2/21/CNO_Cycle.svg/600px-CNO_Cycle.svg.png 2x" data-file-width="1000" data-file-height="1000" /></a><figcaption>Overview of the CNO-I Cycle</figcaption></figure> The proton–proton chain is more prominent in stars the mass of the Sun or less. This difference stems from temperature dependency differences between the two reactions; pp-chain reaction starts at temperatures around 4×106 <a href="/wiki/Kelvin" title="Kelvin">K</a><a href="#cite_note-3">[3]</a> (4 megakelvin), making it the dominant energy source in smaller stars. A self-maintaining CNO chain starts at approximately 15×106 <a href="/wiki/Kelvin" title="Kelvin">K</a>, but its energy output rises much more rapidly with increasing temperatures<a href="#cite_note-salaris_cassini2005-1">[1]</a> so that it becomes the dominant source of energy at approximately 17×106 <a href="/wiki/Kelvin" title="Kelvin">K</a>.<a href="#cite_note-4">[4]</a> The Sun has a <a href="/wiki/Solar_core" title="Solar core">core</a> temperature of around 15.7×106 <a href="/wiki/Kelvin" title="Kelvin">K</a>, and only 1.7% of <a href="/wiki/Helium-4" title="Helium-4">4 He </a> nuclei produced in the Sun are born in the CNO cycle. The <a href="#CNO-I">CNO-I</a> process was independently proposed by <a href="/wiki/Carl_Friedrich_von_Weizs%C3%A4cker" title="Carl Friedrich von Weizsäcker">Carl von Weizsäcker</a><a href="#cite_note-vonWeizsäcker-1-5">[5]</a><a href="#cite_note-vonWeizsäcker-2-6">[6]</a> and <a href="/wiki/Hans_Bethe" title="Hans Bethe">Hans Bethe</a><a href="#cite_note-Bethe-1939-a-7">[7]</a><a href="#cite_note-Bethe-1939-b-8">[8]</a> in the late 1930s. The first reports of the experimental detection of the neutrinos produced by the CNO cycle in the Sun were published in 2020 by the <a href="/wiki/Borexino" title="Borexino">BOREXINO</a> collaboration. This was also the first experimental confirmation that the Sun had a CNO cycle, that the proposed magnitude of the cycle was accurate, and that von Weizsäcker and Bethe were correct.<a href="#cite_note-BOREXINO-2">[2]</a><a href="#cite_note-9">[9]</a><a href="#cite_note-10">[10]</a> <meta property="mw:PageProp/toc" /> <div class="mw-heading mw-heading2"><h2 id="Cold_CNO_cycles">Cold CNO cycles</h2>[<a href="/w/index.php?title=CNO_cycle&action=edit&section=1" title="Edit section: Cold CNO cycles">edit</a>]</div> Under typical conditions found in stars, catalytic hydrogen burning by the CNO cycles is limited by <a href="/wiki/Proton_capture" title="Proton capture">proton captures</a>. Specifically, the timescale for <a href="/wiki/Beta_decay" title="Beta decay">beta decay</a> of the <a href="/wiki/Radionuclide" title="Radionuclide">radioactive nuclei</a> produced is faster than the timescale for fusion. Because of the long timescales involved, the cold CNO cycles convert hydrogen to helium slowly, allowing them to power stars in quiescent equilibrium for many years. <div class="mw-heading mw-heading3"><h3 id="CNO-I">CNO-I</h3>[<a href="/w/index.php?title=CNO_cycle&action=edit&section=2" title="Edit section: CNO-I">edit</a>]</div> The first proposed catalytic cycle for the conversion of hydrogen into helium was initially called the carbon–nitrogen cycle (CN-cycle), also referred to as the Bethe–Weizsäcker cycle in honor of the independent work of <a href="/wiki/Carl_Friedrich_von_Weizs%C3%A4cker" title="Carl Friedrich von Weizsäcker">Carl Friedrich von Weizsäcker</a> in 1937–38<a href="#cite_note-vonWeizsäcker-1-5">[5]</a><a href="#cite_note-vonWeizsäcker-2-6">[6]</a> and <a href="/wiki/Hans_Bethe" title="Hans Bethe">Hans Bethe</a>. Bethe's 1939 papers on the CN-cycle<a href="#cite_note-Bethe-1939-a-7">[7]</a><a href="#cite_note-Bethe-1939-b-8">[8]</a> drew on three earlier papers written in collaboration with <a href="/wiki/Robert_Bacher" title="Robert Bacher">Robert Bacher</a> and <a href="/wiki/Milton_Stanley_Livingston" class="mw-redirect" title="Milton Stanley Livingston">Milton Stanley Livingston</a><a href="#cite_note-11">[11]</a><a href="#cite_note-12">[12]</a><a href="#cite_note-13">[13]</a> and which came to be known informally as Bethe's Bible. It was considered the standard work on nuclear physics for many years and was a significant factor in his being awarded the <a href="/wiki/List_of_Nobel_laureates_in_Physics" title="List of Nobel laureates in Physics">1967 Nobel Prize in Physics</a>.<a href="#cite_note-14">[14]</a> Bethe's original calculations suggested the CN-cycle was the Sun's primary source of energy.<a href="#cite_note-Bethe-1939-a-7">[7]</a><a href="#cite_note-Bethe-1939-b-8">[8]</a> This conclusion arose from a belief that is now known to be mistaken, that the <a href="/wiki/Abundance_of_the_chemical_elements" title="Abundance of the chemical elements">abundance of nitrogen in the sun</a> is approximately 10%; it is actually less than half a percent.<a href="#cite_note-Krane-15">[15]</a> The CN-cycle, named as it contains no stable isotope of oxygen, involves the following cycle of transformations:<a href="#cite_note-Krane-15">[15]</a> <dl><dd><a href="/wiki/Carbon-12" title="Carbon-12">12 6C </a>   →  <a href="/wiki/Nitrogen-13" title="Nitrogen-13">13 7N </a>   →  <a href="/wiki/Carbon-13" title="Carbon-13">13 6C </a>   →   <a href="/wiki/Nitrogen-14" class="mw-redirect" title="Nitrogen-14">14 7N </a>   →   <a href="/wiki/Oxygen-15" class="mw-redirect" title="Oxygen-15">15 8O </a>   →   <a href="/wiki/Nitrogen-15" class="mw-redirect" title="Nitrogen-15">15 7N </a>   →   12 6C </dd></dl> This cycle is now understood as being the first part of a larger process, the CNO-cycle, and the main reactions in this part of the cycle (CNO-I) are:<a href="#cite_note-Krane-15">[15]</a> <dl><dd><table border="0"> <tbody><tr style="height:2em;"> <td>12 6C  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>13 7N  </td> <td>+ </td> <td><a href="/wiki/Gamma_ray" title="Gamma ray"> γ </a> </td> <td> </td> <td> </td> <td>+ </td> <td>1.95 <a href="/wiki/Electronvolt" title="Electronvolt">MeV</a> </td></tr> <tr style="height:2em;"> <td>13 7N  </td> <td> </td> <td> </td> <td>→ </td> <td>13 6C  </td> <td>+ </td> <td><a href="/wiki/Positron" title="Positron"> e+ </a> </td> <td>+ </td> <td><a href="/wiki/Electron_neutrino" title="Electron neutrino"> ν e</a> </td> <td>+ </td> <td>1.20 MeV</td> <td>(<a href="/wiki/Half-life" title="Half-life">half-life</a> of 9.965 minutes<a href="#cite_note-half-life-cn-16">[16]</a>) </td></tr> <tr style="height:2em;"> <td>13 6C  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>14 7N  </td> <td>+ </td> <td> γ  </td> <td> </td> <td> </td> <td>+ </td> <td>7.54 MeV </td></tr> <tr style="height:2em;"> <td>14 7N  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>15 8O  </td> <td>+ </td> <td> γ  </td> <td> </td> <td> </td> <td>+ </td> <td>7.35 MeV </td></tr> <tr style="height:2em;"> <td>15 8O  </td> <td> </td> <td> </td> <td>→ </td> <td>15 7N  </td> <td>+ </td> <td> e+  </td> <td>+ </td> <td> ν e </td> <td>+ </td> <td>1.73 MeV</td> <td>(half-life of 122.24 seconds<a href="#cite_note-half-life-cn-16">[16]</a>) </td></tr> <tr style="height:2em;"> <td>15 7N  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>12 6C  </td> <td>+ </td> <td>4 2He  </td> <td> </td> <td> </td> <td>+ </td> <td>4.96 MeV </td></tr></tbody></table></dd></dl> where the carbon-12 nucleus used in the first reaction is regenerated in the last reaction. After the two <a href="/wiki/Positron_emission" title="Positron emission">positrons emitted</a> <a href="/wiki/Annihilation" title="Annihilation">annihilate</a> with two ambient electrons producing an additional 2.04 MeV, the total energy released in one cycle is 26.73 MeV; in some texts, authors are erroneously including the positron annihilation energy in with the <a href="/wiki/Beta_decay" title="Beta decay">beta-decay</a> <a href="/wiki/Q_value_(nuclear_science)" title="Q value (nuclear science)">Q-value</a> and then neglecting the equal amount of energy released by annihilation, leading to possible confusion. All values are calculated with reference to the Atomic Mass Evaluation 2003.<a href="#cite_note-17">[17]</a> The limiting (slowest) reaction in the CNO-I cycle is the <a href="/wiki/Proton_capture" title="Proton capture">proton capture</a> on 14 7N . In 2006 it was experimentally measured down to stellar energies, revising the calculated age of <a href="/wiki/Globular_cluster" title="Globular cluster">globular clusters</a> by around 1 billion years.<a href="#cite_note-18">[18]</a> The <a href="/wiki/Neutrino" title="Neutrino">neutrinos</a> emitted in beta decay will have a spectrum of energy ranges, because although <a href="/wiki/Conservation_of_momentum#Conservation_of_linear_momentum" class="mw-redirect" title="Conservation of momentum">momentum is conserved</a>, the momentum can be shared in any way between the positron and neutrino, with either emitted at rest and the other taking away the full energy, or anything in between, so long as all the energy from the Q-value is used. The total <a href="/wiki/Momentum" title="Momentum">momentum</a> received by the positron and the neutrino is not great enough to cause a significant recoil of the much <a href="/wiki/Invariant_mass" title="Invariant mass">heavier</a> daughter nucleus<a href="#cite_note-19">[a]</a> and hence, its contribution to kinetic energy of the products, for the precision of values given here, can be neglected. Thus the neutrino emitted during the decay of nitrogen-13 can have an energy from zero up to 1.20 MeV, and the neutrino emitted during the decay of oxygen-15 can have an energy from zero up to 1.73 MeV. On average, about 1.7 MeV of the total energy output is taken away by neutrinos for each loop of the cycle, leaving about 25 MeV available for producing <a href="/wiki/Luminosity" title="Luminosity">luminosity</a>.<a href="#cite_note-20">[19]</a> <div class="mw-heading mw-heading3"><h3 id="CNO-II">CNO-II</h3>[<a href="/w/index.php?title=CNO_cycle&action=edit&section=3" title="Edit section: CNO-II">edit</a>]</div> In a minor branch of the above reaction, occurring in the Sun's core 0.04% of the time, the final reaction involving <a href="/wiki/Nitrogen-15" class="mw-redirect" title="Nitrogen-15">15 7N </a> shown above does not produce carbon-12 and an alpha particle, but instead produces oxygen-16 and a photon and continues <dl><dd><a href="/wiki/Nitrogen-15" class="mw-redirect" title="Nitrogen-15">15 7N </a> → <a href="/wiki/Oxygen-16" title="Oxygen-16">16 8O </a> → <a href="/wiki/Fluorine-17" class="mw-redirect" title="Fluorine-17">17 9F </a> → <a href="/wiki/Oxygen-17" title="Oxygen-17">17 8O </a> → <a href="/wiki/Nitrogen-14" class="mw-redirect" title="Nitrogen-14">14 7N </a> → <a href="/wiki/Oxygen-15" class="mw-redirect" title="Oxygen-15">15 8O </a> → 15 7N </dd></dl> In detail: <dl><dd><table border="0"> <tbody><tr style="height:2em;"> <td>15 7N  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>16 8O  </td> <td>+ </td> <td> γ  </td> <td> </td> <td> </td> <td>+ </td> <td>12.13 MeV </td></tr> <tr style="height:2em;"> <td>16 8O  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>17 9F  </td> <td>+ </td> <td> γ  </td> <td> </td> <td> </td> <td>+ </td> <td>0.60 MeV </td></tr> <tr style="height:2em;"> <td>17 9F  </td> <td> </td> <td> </td> <td>→ </td> <td>17 8O  </td> <td>+ </td> <td> e+  </td> <td>+ </td> <td> ν e </td> <td>+ </td> <td>2.76 MeV</td> <td>(half-life of 64.49 seconds) </td></tr> <tr style="height:2em;"> <td>17 8O  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>14 7N  </td> <td>+ </td> <td>4 2He  </td> <td> </td> <td> </td> <td>+ </td> <td>1.19 MeV </td></tr> <tr style="height:2em;"> <td>14 7N  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>15 8O  </td> <td>+ </td> <td> γ  </td> <td> </td> <td> </td> <td>+ </td> <td>7.35 MeV </td></tr> <tr style="height:2em;"> <td>15 8O  </td> <td> </td> <td> </td> <td>→ </td> <td>15 7N  </td> <td>+ </td> <td> e+  </td> <td>+ </td> <td> ν e </td> <td>+ </td> <td>2.75 MeV</td> <td>(half-life of 122.24 seconds) </td></tr></tbody></table></dd></dl> Like the carbon, nitrogen, and oxygen involved in the main branch, the <a href="/wiki/Fluorine" title="Fluorine">fluorine</a> produced in the minor branch is merely an intermediate product; at steady state, it does not accumulate in the star. <div class="mw-heading mw-heading3"><h3 id="CNO-III">CNO-III</h3>[<a href="/w/index.php?title=CNO_cycle&action=edit&section=4" title="Edit section: CNO-III">edit</a>]</div> This subdominant branch is significant only for massive stars. The reactions are started when one of the reactions in CNO-II results in fluorine-18 and a photon instead of nitrogen-14 and an alpha particle, and continues <dl><dd><a href="/wiki/Oxygen-17" title="Oxygen-17">17 8O </a> → <a href="/wiki/Fluorine-18" title="Fluorine-18">18 9F </a> → <a href="/wiki/Oxygen-18" title="Oxygen-18">18 8O </a> → <a href="/wiki/Nitrogen-15" class="mw-redirect" title="Nitrogen-15">15 7N </a> → <a href="/wiki/Oxygen-16" title="Oxygen-16">16 8O </a> → <a href="/wiki/Fluorine-17" class="mw-redirect" title="Fluorine-17">17 9F </a> → 17 8O </dd></dl> In detail: <dl><dd><table border="0"> <tbody><tr style="height:2em;"> <td>17 8O  </td> <td>+  </td> <td>1 1H  </td> <td>→  </td> <td>18 9F  </td> <td>+  </td> <td> γ  </td> <td> </td> <td> </td> <td>+  </td> <td>5.61 MeV </td></tr> <tr style="height:2em;"> <td>18 9F  </td> <td> </td> <td> </td> <td>→  </td> <td>18 8O  </td> <td>+  </td> <td> e+  </td> <td>+  </td> <td> ν e  </td> <td>+  </td> <td>1.656 MeV</td> <td>(half-life of 109.771 min) </td></tr> <tr style="height:2em;"> <td>18 8O  </td> <td>+  </td> <td>1 1H  </td> <td>→  </td> <td>15 7N  </td> <td>+  </td> <td>4 2He  </td> <td> </td> <td> </td> <td>+  </td> <td>3.98 MeV </td></tr> <tr style="height:2em;"> <td>15 7N  </td> <td>+  </td> <td>1 1H  </td> <td>→  </td> <td>16 8O  </td> <td>+  </td> <td> γ  </td> <td> </td> <td> </td> <td>+  </td> <td>12.13 MeV </td></tr> <tr style="height:2em;"> <td>16 8O  </td> <td>+  </td> <td>1 1H  </td> <td>→  </td> <td>17 9F  </td> <td>+  </td> <td> γ  </td> <td> </td> <td> </td> <td>+  </td> <td>0.60 MeV </td></tr> <tr style="height:2em;"> <td>17 9F  </td> <td> </td> <td> </td> <td>→  </td> <td>17 8O  </td> <td>+  </td> <td> e+  </td> <td>+  </td> <td> ν e  </td> <td>+  </td> <td>2.76 MeV</td> <td>(half-life of 64.49 s) </td></tr></tbody></table></dd></dl> <div class="mw-heading mw-heading3"><h3 id="CNO-IV">CNO-IV</h3>[<a href="/w/index.php?title=CNO_cycle&action=edit&section=5" title="Edit section: CNO-IV">edit</a>]</div> <figure class="mw-default-size" typeof="mw:File/Thumb"><a href="/wiki/File:NuclearReaction.svg" class="mw-file-description"><img src="//upload.wikimedia.org/wikipedia/commons/thumb/4/4b/NuclearReaction.svg/220px-NuclearReaction.svg.png" decoding="async" width="220" height="140" class="mw-file-element" srcset="//upload.wikimedia.org/wikipedia/commons/thumb/4/4b/NuclearReaction.svg/330px-NuclearReaction.svg.png 1.5x, //upload.wikimedia.org/wikipedia/commons/thumb/4/4b/NuclearReaction.svg/440px-NuclearReaction.svg.png 2x" data-file-width="550" data-file-height="350" /></a><figcaption>A proton reacts with a nucleus causing release of an alpha particle.</figcaption></figure> Like the CNO-III, this branch is also only significant in massive stars. The reactions are started when one of the reactions in CNO-III results in fluorine-19 and a photon instead of nitrogen-15 and an alpha particle, and continues <dl><dd><a href="/wiki/Oxygen-18" title="Oxygen-18">18 8O </a> → <a href="/wiki/Fluorine-19" class="mw-redirect" title="Fluorine-19">19 9F </a> → <a href="/wiki/Oxygen-16" title="Oxygen-16">16 8O </a> → <a href="/wiki/Fluorine-17" class="mw-redirect" title="Fluorine-17">17 9F </a> → <a href="/wiki/Oxygen-17" title="Oxygen-17">17 8O </a> → <a href="/wiki/Fluorine-18" title="Fluorine-18">18 9F </a> → <a href="/wiki/Oxygen-18" title="Oxygen-18">18 8O </a></dd></dl> In detail: <dl><dd><table border="0"> <tbody><tr> <td>18 8O  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>19 9F  </td> <td>+ </td> <td> γ  </td> <td> </td> <td> </td> <td>+ </td> <td>7.994 MeV </td></tr> <tr> <td>19 9F  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>16 8O  </td> <td>+ </td> <td>4 2He  </td> <td> </td> <td> </td> <td>+ </td> <td>8.114 MeV </td></tr> <tr style="height:2em;"> <td>16 8O  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>17 9F  </td> <td>+ </td> <td> γ  </td> <td> </td> <td> </td> <td>+ </td> <td>0.60 MeV </td></tr> <tr style="height:2em;"> <td>17 9F  </td> <td> </td> <td> </td> <td>→ </td> <td>17 8O  </td> <td>+ </td> <td> e+  </td> <td>+ </td> <td> ν e </td> <td>+ </td> <td>2.76 MeV</td> <td>(half-life of 64.49 seconds) </td></tr> <tr style="height:2em;"> <td>17 8O  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>18 9F  </td> <td>+ </td> <td> γ  </td> <td> </td> <td> </td> <td>+ </td> <td>5.61 MeV </td></tr> <tr style="height:2em;"> <td>18 9F  </td> <td> </td> <td> </td> <td>→ </td> <td>18 8O  </td> <td>+ </td> <td> e+  </td> <td>+ </td> <td> ν e </td> <td>+ </td> <td>1.656 MeV</td> <td>(half-life of 109.771 minutes) </td></tr> </tbody></table></dd></dl> In some instances 18 9F can combine with a helium nucleus to start a sodium-neon cycle.<a href="#cite_note-21">[20]</a> <div class="mw-heading mw-heading2"><h2 id="Hot_CNO_cycles">Hot CNO cycles</h2>[<a href="/w/index.php?title=CNO_cycle&action=edit&section=6" title="Edit section: Hot CNO cycles">edit</a>]</div> Under conditions of higher temperature and pressure, such as those found in <a href="/wiki/Nova" title="Nova">novae</a> and <a href="/wiki/X-ray_burster" title="X-ray burster">X-ray bursts</a>, the rate of proton captures exceeds the rate of beta-decay, pushing the burning to the <a href="/wiki/Nuclear_drip_line" title="Nuclear drip line">proton drip line</a>. The essential idea is that a radioactive species will capture a proton before it can beta decay, opening new nuclear burning pathways that are otherwise inaccessible. Because of the higher temperatures involved, these catalytic cycles are typically referred to as the hot CNO cycles; because the timescales are limited by beta decays instead of <a href="/wiki/Proton_capture" title="Proton capture">proton captures</a>, they are also called the beta-limited CNO cycles.[<a href="/wiki/Wikipedia:Please_clarify" title="Wikipedia:Please clarify">clarification needed</a>] <div class="mw-heading mw-heading3"><h3 id="HCNO-I">HCNO-I</h3>[<a href="/w/index.php?title=CNO_cycle&action=edit&section=7" title="Edit section: HCNO-I">edit</a>]</div> The difference between the CNO-I cycle and the HCNO-I cycle is that <a href="/wiki/Nitrogen-13" title="Nitrogen-13">13 7N </a> captures a proton instead of decaying, leading to the total sequence <dl><dd><a href="/wiki/Carbon-12" title="Carbon-12">12 6C </a>→<a href="/wiki/Nitrogen-13" title="Nitrogen-13">13 7N </a>→<a href="/wiki/Oxygen-14" class="mw-redirect" title="Oxygen-14">14 8O </a>→<a href="/wiki/Nitrogen-14" class="mw-redirect" title="Nitrogen-14">14 7N </a>→<a href="/wiki/Oxygen-15" class="mw-redirect" title="Oxygen-15">15 8O </a>→<a href="/wiki/Nitrogen-15" class="mw-redirect" title="Nitrogen-15">15 7N </a>→12 6C </dd></dl> In detail: <dl><dd><table border="0"> <tbody><tr style="height:2em;"> <td>12 6C  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>13 7N  </td> <td>+ </td> <td><a href="/wiki/Gamma_ray" title="Gamma ray"> γ </a> </td> <td> </td> <td> </td> <td>+ </td> <td>1.95 <a href="/wiki/Electronvolt" title="Electronvolt">MeV</a> </td></tr> <tr style="height:2em;"> <td>13 7N  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>14 8O  </td> <td>+ </td> <td> γ  </td> <td> </td> <td> </td> <td>+ </td> <td>4.63 MeV </td></tr> <tr style="height:2em;"> <td>14 8O  </td> <td> </td> <td> </td> <td>→ </td> <td>14 7N  </td> <td>+ </td> <td><a href="/wiki/Positron" title="Positron"> e+ </a> </td> <td>+ </td> <td><a href="/wiki/Electron_neutrino" title="Electron neutrino"> ν e</a> </td> <td>+ </td> <td>5.14 MeV</td> <td>(<a href="/wiki/Half-life" title="Half-life">half-life</a> of 70.641 seconds) </td></tr> <tr style="height:2em;"> <td>14 7N  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>15 8O  </td> <td>+ </td> <td> γ  </td> <td> </td> <td> </td> <td>+ </td> <td>7.35 MeV </td></tr> <tr style="height:2em;"> <td>15 8O  </td> <td> </td> <td> </td> <td>→ </td> <td>15 7N  </td> <td>+ </td> <td> e+  </td> <td>+ </td> <td> ν e </td> <td>+ </td> <td>2.75 MeV</td> <td>(half-life of 122.24 seconds) </td></tr> <tr style="height:2em;"> <td>15 7N  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>12 6C  </td> <td>+ </td> <td>4 2He  </td> <td> </td> <td> </td> <td>+ </td> <td>4.96 MeV </td></tr></tbody></table></dd></dl> <div class="mw-heading mw-heading3"><h3 id="HCNO-II">HCNO-II</h3>[<a href="/w/index.php?title=CNO_cycle&action=edit&section=8" title="Edit section: HCNO-II">edit</a>]</div> The notable difference between the CNO-II cycle and the HCNO-II cycle is that <a href="/wiki/Fluorine-17" class="mw-redirect" title="Fluorine-17">17 9F </a> captures a proton instead of decaying, and neon is produced in a subsequent reaction on <a href="/wiki/Fluorine-18" title="Fluorine-18">18 9F </a>, leading to the total sequence <dl><dd><a href="/wiki/Nitrogen-15" class="mw-redirect" title="Nitrogen-15">15 7N </a>→<a href="/wiki/Oxygen-16" title="Oxygen-16">16 8O </a>→<a href="/wiki/Fluorine-17" class="mw-redirect" title="Fluorine-17">17 9F </a>→<a href="/wiki/Neon-18" class="mw-redirect" title="Neon-18">18 10Ne </a>→<a href="/wiki/Fluorine-18" title="Fluorine-18">18 9F </a>→<a href="/wiki/Oxygen-15" class="mw-redirect" title="Oxygen-15">15 8O </a>→15 7N </dd></dl> In detail: <dl><dd><table border="0"> <tbody><tr style="height:2em;"> <td>15 7N  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>16 8O  </td> <td>+ </td> <td> γ  </td> <td> </td> <td> </td> <td>+ </td> <td>12.13 MeV </td></tr> <tr style="height:2em;"> <td>16 8O  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>17 9F  </td> <td>+ </td> <td> γ  </td> <td> </td> <td> </td> <td>+ </td> <td>0.60 MeV </td></tr> <tr style="height:2em;"> <td>17 9F  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>18 10Ne  </td> <td>+ </td> <td> γ  </td> <td> </td> <td> </td> <td>+ </td> <td>3.92 MeV </td></tr> <tr style="height:2em;"> <td>18 10Ne  </td> <td> </td> <td> </td> <td>→ </td> <td>18 9F  </td> <td>+ </td> <td> e+  </td> <td>+ </td> <td> ν e </td> <td>+ </td> <td>4.44 MeV</td> <td>(half-life of 1.672 seconds) </td></tr> <tr style="height:2em;"> <td>18 9F  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>15 8O  </td> <td>+ </td> <td>4 2He  </td> <td> </td> <td> </td> <td>+ </td> <td>2.88 MeV </td></tr> <tr style="height:2em;"> <td>15 8O  </td> <td> </td> <td> </td> <td>→ </td> <td>15 7N  </td> <td>+ </td> <td> e+  </td> <td>+ </td> <td> ν e </td> <td>+ </td> <td>2.75 MeV</td> <td>(half-life of 122.24 seconds) </td></tr></tbody></table></dd></dl> <div class="mw-heading mw-heading3"><h3 id="HCNO-III">HCNO-III</h3>[<a href="/w/index.php?title=CNO_cycle&action=edit&section=9" title="Edit section: HCNO-III">edit</a>]</div> An alternative to the HCNO-II cycle is that <a href="/wiki/Fluorine-18" title="Fluorine-18">18 9F </a> captures a proton moving towards higher mass and using the same helium production mechanism as the CNO-IV cycle as <dl><dd>18 9F →<a href="/wiki/Neon-19" class="mw-redirect" title="Neon-19">19 10Ne </a>→<a href="/wiki/Fluorine-19" class="mw-redirect" title="Fluorine-19">19 9F </a>→<a href="/wiki/Oxygen-16" title="Oxygen-16">16 8O </a>→<a href="/wiki/Fluorine-17" class="mw-redirect" title="Fluorine-17">17 9F </a>→<a href="/wiki/Neon-18" class="mw-redirect" title="Neon-18">18 10Ne </a>→18 9F </dd></dl> In detail: <dl><dd><table border="0"> <tbody><tr style="height:2em;"> <td>18 9F  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>19 10Ne  </td> <td>+ </td> <td> γ  </td> <td> </td> <td> </td> <td>+ </td> <td>6.41 MeV </td></tr> <tr style="height:2em;"> <td>19 10Ne  </td> <td> </td> <td> </td> <td>→ </td> <td>19 9F  </td> <td>+ </td> <td> e+  </td> <td>+ </td> <td> ν e </td> <td>+ </td> <td>3.32 MeV</td> <td>(half-life of 17.22 seconds) </td></tr> <tr style="height:2em;"> <td>19 9F  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>16 8O  </td> <td>+ </td> <td>4 2He  </td> <td> </td> <td> </td> <td>+ </td> <td>8.11 MeV </td></tr> <tr style="height:2em;"> <td>16 8O  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>17 9F  </td> <td>+ </td> <td> γ  </td> <td> </td> <td> </td> <td>+ </td> <td>0.60 MeV </td></tr> <tr style="height:2em;"> <td>17 9F  </td> <td>+ </td> <td>1 1H  </td> <td>→ </td> <td>18 10Ne  </td> <td>+ </td> <td> γ  </td> <td> </td> <td> </td> <td>+ </td> <td>3.92 MeV </td></tr> <tr style="height:2em;"> <td>18 10Ne  </td> <td> </td> <td> </td> <td>→ </td> <td>18 9F  </td> <td>+ </td> <td> e+  </td> <td>+ </td> <td> ν e </td> <td>+ </td> <td>4.44 MeV</td> <td>(half-life of 1.672 seconds) </td></tr></tbody></table></dd></dl> <div class="mw-heading mw-heading2"><h2 id="Use_in_astronomy">Use in astronomy</h2>[<a href="/w/index.php?title=CNO_cycle&action=edit&section=10" title="Edit section: Use in astronomy">edit</a>]</div> While the total number of "catalytic" nuclei are conserved in the cycle, in <a href="/wiki/Stellar_evolution" title="Stellar evolution">stellar evolution</a> the relative proportions of the nuclei are altered. When the cycle is run to equilibrium, the ratio of the carbon-12/carbon-13 nuclei is driven to 3.5, and nitrogen-14 becomes the most numerous nucleus, regardless of initial composition. During a star's evolution, convective mixing episodes moves material, within which the CNO cycle has operated, from the star's interior to the surface, altering the observed composition of the star. <a href="/wiki/Red_giant" title="Red giant">Red giant</a> stars are observed to have lower carbon-12/carbon-13 and carbon-12/nitrogen-14 ratios than do <a href="/wiki/Main_sequence" title="Main sequence">main sequence</a> stars, which is considered to be convincing evidence for the operation of the CNO cycle.<a href="#cite_note-Mar98-22">[21]</a> <div class="mw-heading mw-heading2"><h2 id="See_also">See also</h2>[<a href="/w/index.php?title=CNO_cycle&action=edit&section=11" title="Edit section: See also">edit</a>]</div> <ul><li><a href="/wiki/Aneutronic_fusion" title="Aneutronic fusion">Aneutronic fusion</a></li> <li><a href="/wiki/Cold_fusion" title="Cold fusion">Cold fusion</a></li> <li><a href="/wiki/Fusion_power" title="Fusion power">Fusion power</a></li> <li><a href="/wiki/Nuclear_fusion" title="Nuclear fusion">Nuclear fusion</a></li> <li><a href="/wiki/Proton%E2%80%93proton_chain" title="Proton–proton chain">Proton–proton chain</a>, as found in stars like the Sun</li> <li><a href="/wiki/Stellar_nucleosynthesis" title="Stellar nucleosynthesis">Stellar nucleosynthesis</a>, the whole topic</li> <li><a href="/wiki/Triple-alpha_process" title="Triple-alpha process">Triple-alpha process</a>, how 12 C is produced from lighter nuclei</li></ul> <div class="mw-heading mw-heading2"><h2 id="Footnotes">Footnotes</h2>[<a href="/w/index.php?title=CNO_cycle&action=edit&section=12" title="Edit section: Footnotes">edit</a>]</div> <style data-mw-deduplicate="TemplateStyles:r1239543626">.mw-parser-output .reflist{margin-bottom:0.5em;list-style-type:decimal}@media screen{.mw-parser-output .reflist{font-size:90%}}.mw-parser-output .reflist .references{font-size:100%;margin-bottom:0;list-style-type:inherit}.mw-parser-output .reflist-columns-2{column-width:30em}.mw-parser-output .reflist-columns-3{column-width:25em}.mw-parser-output .reflist-columns{margin-top:0.3em}.mw-parser-output .reflist-columns ol{margin-top:0}.mw-parser-output .reflist-columns li{page-break-inside:avoid;break-inside:avoid-column}.mw-parser-output .reflist-upper-alpha{list-style-type:upper-alpha}.mw-parser-output .reflist-upper-roman{list-style-type:upper-roman}.mw-parser-output .reflist-lower-alpha{list-style-type:lower-alpha}.mw-parser-output .reflist-lower-greek{list-style-type:lower-greek}.mw-parser-output .reflist-lower-roman{list-style-type:lower-roman}</style><div class="reflist reflist-lower-alpha"> <div class="mw-references-wrap"><ol class="references"> <li id="cite_note-19"><a href="#cite_ref-19">^</a> Note: It is not important how invariant masses of e and ν are small, because they are already small enough to become relativistic. What is important is that the daughter nucleus is heavy compared to <style data-mw-deduplicate="TemplateStyles:r1154941027">.mw-parser-output .frac{white-space:nowrap}.mw-parser-output .frac .num,.mw-parser-output .frac .den{font-size:80%;line-height:0;vertical-align:super}.mw-parser-output .frac .den{vertical-align:sub}.mw-parser-output .sr-only{border:0;clip:rect(0,0,0,0);clip-path:polygon(0px 0px,0px 0px,0px 0px);height:1px;margin:-1px;overflow:hidden;padding:0;position:absolute;width:1px}</style>p⁄c . </li> </ol></div></div> <div class="mw-heading mw-heading2"><h2 id="References">References</h2>[<a href="/w/index.php?title=CNO_cycle&action=edit&section=13" title="Edit section: References">edit</a>]</div> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1239543626"><div class="reflist"> <div class="mw-references-wrap mw-references-columns"><ol class="references"> <li id="cite_note-salaris_cassini2005-1">^ <a href="#cite_ref-salaris_cassini2005_1-0">a</a> <a href="#cite_ref-salaris_cassini2005_1-1">b</a> <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="CITEREFSalarisCassisi2005" class="citation book cs1">Salaris, Maurizio; Cassisi, Santi (2005). <a rel="nofollow" class="external text" href="https://archive.org/details/evolutionofstars0000sala">Evolution of Stars and Stellar Populations</a>. <a href="/wiki/John_Wiley_and_Sons" class="mw-redirect" title="John Wiley and Sons">John Wiley and Sons</a>. pp. <a rel="nofollow" class="external text" href="https://archive.org/details/evolutionofstars0000sala/page/119">119</a>–121. <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/0-470-09220-3" title="Special:BookSources/0-470-09220-3"><bdi>0-470-09220-3</bdi></a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Evolution+of+Stars+and+Stellar+Populations&rft.pages=119-121&rft.pub=John+Wiley+and+Sons&rft.date=2005&rft.isbn=0-470-09220-3&rft.aulast=Salaris&rft.aufirst=Maurizio&rft.au=Cassisi%2C+Santi&rft_id=https%3A%2F%2Farchive.org%2Fdetails%2Fevolutionofstars0000sala&rfr_id=info%3Asid%2Fen.wikipedia.org%3ACNO+cycle" class="Z3988"> </li> <li id="cite_note-BOREXINO-2">^ <a href="#cite_ref-BOREXINO_2-0">a</a> <a href="#cite_ref-BOREXINO_2-1">b</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFAgostiniAltenmüllerAppelAtroshchenko2020" class="citation journal cs1">Agostini, M.; Altenmüller, K.; et al. 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Nature. 587 (7835): 577–582. <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<a rel="nofollow" class="external text" href="https://arxiv.org/abs/2006.15115">2006.15115</a>. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2020Natur.587..577B">2020Natur.587..577B</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1038%2Fs41586-020-2934-0">10.1038/s41586-020-2934-0</a>. <a href="/wiki/ISSN_(identifier)" class="mw-redirect" title="ISSN (identifier)">ISSN</a> <a rel="nofollow" class="external text" href="https://search.worldcat.org/issn/1476-4687">1476-4687</a>. <a href="/wiki/PMID_(identifier)" class="mw-redirect" title="PMID (identifier)">PMID</a> <a rel="nofollow" class="external text" href="https://pubmed.ncbi.nlm.nih.gov/33239797">33239797</a>. <a href="/wiki/S2CID_(identifier)" class="mw-redirect" title="S2CID (identifier)">S2CID</a> <a rel="nofollow" class="external text" href="https://api.semanticscholar.org/CorpusID:227174644">227174644</a>. <q>This result therefore paves the way towards a direct measurement of the solar metallicity using CNO neutrinos. 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Atomic Mass Data Center. Archived from <a rel="nofollow" class="external text" href="http://amdc.in2p3.fr/web/masseval.html">the original</a> on 28 September 2011. Retrieved 25 October 2011.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=The+2003+Atomic+Mass+Evaluation&rft.pub=Atomic+Mass+Data+Center&rft.date=2003-11-18&rft.aulast=Wapstra&rft.aufirst=Aaldert&rft.au=Audi%2C+Georges&rft_id=http%3A%2F%2Famdc.in2p3.fr%2Fweb%2Fmasseval.html&rfr_id=info%3Asid%2Fen.wikipedia.org%3ACNO+cycle" class="Z3988"> </li> <li id="cite_note-18"><a href="#cite_ref-18">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFLemutBemmererConfortolaBonetti2006" class="citation journal cs1">Lemut, A.; Bemmerer, D.; Confortola, F.; Bonetti, R.; Broggini, C.; Corvisiero, P.; et al. (LUNA Collaboration) (2006). "First measurement of the 14N(p,γ)15O cross section down to 70 keV". <a href="/wiki/Physics_Letters_B" class="mw-redirect" title="Physics Letters B">Physics Letters B</a>. 634 (5–6): 483–487. <a href="/wiki/ArXiv_(identifier)" class="mw-redirect" title="ArXiv (identifier)">arXiv</a>:<a rel="nofollow" class="external text" href="https://arxiv.org/abs/nucl-ex/0602012">nucl-ex/0602012</a>. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/2006PhLB..634..483L">2006PhLB..634..483L</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1016%2Fj.physletb.2006.02.021">10.1016/j.physletb.2006.02.021</a>. <a href="/wiki/S2CID_(identifier)" class="mw-redirect" title="S2CID (identifier)">S2CID</a> <a rel="nofollow" class="external text" href="https://api.semanticscholar.org/CorpusID:16875233">16875233</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Physics+Letters+B&rft.atitle=First+measurement+of+the+%3Csup%3E14%3C%2Fsup%3EN%28p%2C%CE%B3%29%3Csup%3E15%3C%2Fsup%3EO+cross+section+down+to+70+keV&rft.volume=634&rft.issue=5%E2%80%936&rft.pages=483-487&rft.date=2006&rft_id=info%3Aarxiv%2Fnucl-ex%2F0602012&rft_id=https%3A%2F%2Fapi.semanticscholar.org%2FCorpusID%3A16875233%23id-name%3DS2CID&rft_id=info%3Adoi%2F10.1016%2Fj.physletb.2006.02.021&rft_id=info%3Abibcode%2F2006PhLB..634..483L&rft.aulast=Lemut&rft.aufirst=A.&rft.au=Bemmerer%2C+D.&rft.au=Confortola%2C+F.&rft.au=Bonetti%2C+R.&rft.au=Broggini%2C+C.&rft.au=Corvisiero%2C+P.&rft.au=Costantini%2C+H.&rft.au=Cruz%2C+J.&rft.au=Formicola%2C+A.&rft.au=F%C3%BCl%C3%B6p%2C+Zs.&rft.au=Gervino%2C+G.&rft.au=Guglielmetti%2C+A.&rft.au=Gustavino%2C+C.&rft.au=Gy%C3%BCrky%2C+Gy.&rft.au=Imbriani%2C+G.&rft.au=Jesus+A.%2C+P.&rft.au=Junker%2C+M.&rft.au=Limata%2C+B.&rft.au=Menegazzo%2C+R.&rft.au=Prati%2C+P.&rft.au=Roca%2C+V.&rft.au=Rogalla%2C+D.&rft.au=Rolfs%2C+C.&rft.au=Romano%2C+M.&rft.au=Rossi+Alvarez%2C+C.&rft.au=Sch%C3%BCmann%2C+F.&rft.au=Somorjai%2C+E.&rft.au=Straniero%2C+O.&rft.au=Strieder%2C+F.&rft.au=Terrasi%2C+F.&rft.au=Trautvetter%2C+H.P.&rfr_id=info%3Asid%2Fen.wikipedia.org%3ACNO+cycle" class="Z3988"> </li> <li id="cite_note-20"><a href="#cite_ref-20">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFSchefflerElsässer1990" class="citation book cs1">Scheffler, Helmut; Elsässer, Hans (1990). Die Physik der Sterne und der Sonne [The Physics of the Stars and the Sun]. <a href="/wiki/Bibliographisches_Institut" title="Bibliographisches Institut">Bibliographisches Institut</a> (Mannheim, Wien, Zürich). <a href="/wiki/ISBN_(identifier)" class="mw-redirect" title="ISBN (identifier)">ISBN</a> <a href="/wiki/Special:BookSources/3-411-14172-7" title="Special:BookSources/3-411-14172-7"><bdi>3-411-14172-7</bdi></a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=book&rft.btitle=Die+Physik+der+Sterne+und+der+Sonne&rft.pub=Bibliographisches+Institut+%28Mannheim%2C+Wien%2C+Z%C3%BCrich%29&rft.date=1990&rft.isbn=3-411-14172-7&rft.aulast=Scheffler&rft.aufirst=Helmut&rft.au=Els%C3%A4sser%2C+Hans&rfr_id=info%3Asid%2Fen.wikipedia.org%3ACNO+cycle" class="Z3988"> </li> <li id="cite_note-21"><a href="#cite_ref-21">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFDepalo" class="citation web cs1">Depalo, Rosanna. <a rel="nofollow" class="external text" href="https://web.archive.org/web/20200728182717/https://core.ac.uk/download/pdf/31144835.pdf">"The neon-sodium cycle: Study of the 22Ne(p, γ)23Na reaction at astrophysical energies"</a> (PDF). Archived from <a rel="nofollow" class="external text" href="https://core.ac.uk/download/pdf/31144835.pdf">the original</a> (PDF) on 28 July 2020. Retrieved 16 April 2020.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Abook&rft.genre=unknown&rft.btitle=The+neon-sodium+cycle%3A+Study+of+the+22Ne%28p%2C+%CE%B3%2923Na+reaction+at+astrophysical+energies&rft.aulast=Depalo&rft.aufirst=Rosanna&rft_id=https%3A%2F%2Fcore.ac.uk%2Fdownload%2Fpdf%2F31144835.pdf&rfr_id=info%3Asid%2Fen.wikipedia.org%3ACNO+cycle" class="Z3988"> </li> <li id="cite_note-Mar98-22"><a href="#cite_ref-Mar98_22-0">^</a> <link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFMarks_and_Sarna1998" class="citation journal cs1">Marks and Sarna (December 1998). <a rel="nofollow" class="external text" href="https://doi.org/10.1046%2Fj.1365-8711.1998.02039.x">"The chemical evolution of the secondary stars in close binaries, arising from common-envelope evolution and nova outbursts"</a>. Monthly Notices of the Royal Astronomical Society. 301 (3): 699–720. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1998MNRAS.301..699M">1998MNRAS.301..699M</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1046%2Fj.1365-8711.1998.02039.x">10.1046/j.1365-8711.1998.02039.x</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Monthly+Notices+of+the+Royal+Astronomical+Society&rft.atitle=The+chemical+evolution+of+the+secondary+stars+in+close+binaries%2C+arising+from+common-envelope+evolution+and+nova+outbursts&rft.volume=301&rft.issue=3&rft.pages=699-720&rft.date=1998-12&rft_id=info%3Adoi%2F10.1046%2Fj.1365-8711.1998.02039.x&rft_id=info%3Abibcode%2F1998MNRAS.301..699M&rft.au=Marks+and+Sarna&rft_id=https%3A%2F%2Fdoi.org%2F10.1046%252Fj.1365-8711.1998.02039.x&rfr_id=info%3Asid%2Fen.wikipedia.org%3ACNO+cycle" class="Z3988"> </li> </ol></div></div> <div class="mw-heading mw-heading2"><h2 id="Further_reading">Further reading</h2>[<a href="/w/index.php?title=CNO_cycle&action=edit&section=14" title="Edit section: Further reading">edit</a>]</div> <ul><li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFBethe1939" class="citation journal cs1">Bethe, H. A. (1939). <a rel="nofollow" class="external text" href="https://doi.org/10.1103%2FPhysRev.55.434">"Energy Production in Stars"</a>. <a href="/wiki/Physical_Review" title="Physical Review">Physical Review</a>. 55 (5): 434–56. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1939PhRv...55..434B">1939PhRv...55..434B</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1103%2FPhysRev.55.434">10.1103/PhysRev.55.434</a>. <a href="/wiki/PMID_(identifier)" class="mw-redirect" title="PMID (identifier)">PMID</a> <a rel="nofollow" class="external text" href="https://pubmed.ncbi.nlm.nih.gov/17835673">17835673</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Physical+Review&rft.atitle=Energy+Production+in+Stars&rft.volume=55&rft.issue=5&rft.pages=434-56&rft.date=1939&rft_id=info%3Apmid%2F17835673&rft_id=info%3Adoi%2F10.1103%2FPhysRev.55.434&rft_id=info%3Abibcode%2F1939PhRv...55..434B&rft.aulast=Bethe&rft.aufirst=H.+A.&rft_id=https%3A%2F%2Fdoi.org%2F10.1103%252FPhysRev.55.434&rfr_id=info%3Asid%2Fen.wikipedia.org%3ACNO+cycle" class="Z3988"></li> <li><link rel="mw-deduplicated-inline-style" href="mw-data:TemplateStyles:r1238218222"><cite id="CITEREFIben1967" class="citation journal cs1">Iben, I. (1967). "Stellar Evolution Within and off the Main Sequence". <a href="/wiki/Annual_Review_of_Astronomy_and_Astrophysics" title="Annual Review of Astronomy and Astrophysics">Annual Review of Astronomy and Astrophysics</a>. 5: 571–626. <a href="/wiki/Bibcode_(identifier)" class="mw-redirect" title="Bibcode (identifier)">Bibcode</a>:<a rel="nofollow" class="external text" href="https://ui.adsabs.harvard.edu/abs/1967ARA&A...5..571I">1967ARA&A...5..571I</a>. <a href="/wiki/Doi_(identifier)" class="mw-redirect" title="Doi (identifier)">doi</a>:<a rel="nofollow" class="external text" href="https://doi.org/10.1146%2Fannurev.aa.05.090167.003035">10.1146/annurev.aa.05.090167.003035</a>.</cite><span title="ctx_ver=Z39.88-2004&rft_val_fmt=info%3Aofi%2Ffmt%3Akev%3Amtx%3Ajournal&rft.genre=article&rft.jtitle=Annual+Review+of+Astronomy+and+Astrophysics&rft.atitle=Stellar+Evolution+Within+and+off+the+Main+Sequence&rft.volume=5&rft.pages=571-626&rft.date=1967&rft_id=info%3Adoi%2F10.1146%2Fannurev.aa.05.090167.003035&rft_id=info%3Abibcode%2F1967ARA%26A...5..571I&rft.aulast=Iben&rft.aufirst=I.&rfr_id=info%3Asid%2Fen.wikipedia.org%3ACNO+cycle" class="Z3988"></li></ul> <div class="navbox-styles"><style data-mw-deduplicate="TemplateStyles:r1129693374">.mw-parser-output .hlist dl,.mw-parser-output .hlist ol,.mw-parser-output .hlist ul{margin:0;padding:0}.mw-parser-output .hlist dd,.mw-parser-output .hlist dt,.mw-parser-output .hlist li{margin:0;display:inline}.mw-parser-output .hlist.inline,.mw-parser-output .hlist.inline dl,.mw-parser-output .hlist.inline ol,.mw-parser-output .hlist.inline ul,.mw-parser-output .hlist dl dl,.mw-parser-output .hlist dl ol,.mw-parser-output .hlist dl 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href="/wiki/Electron_capture" title="Electron capture">Electron capture</a> <ul><li><a href="/wiki/Double_electron_capture" title="Double electron capture">Double</a></li></ul></li> <li><a href="/wiki/Internal_conversion" title="Internal conversion">Internal conversion</a></li> <li><a href="/wiki/Isomeric_transition" class="mw-redirect" title="Isomeric transition">Isomeric transition</a></li> <li><a href="/wiki/Neutron_emission" title="Neutron emission">Neutron emission</a></li> <li><a href="/wiki/Positron_emission" title="Positron emission">Positron emission</a></li> <li><a href="/wiki/Proton_emission" title="Proton emission">Proton emission</a></li> <li><a href="/wiki/Spontaneous_fission" title="Spontaneous fission">Spontaneous fission</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%"><a href="/wiki/Stellar_nucleosynthesis" title="Stellar nucleosynthesis">Stellar nucleosynthesis</a></th><td class="navbox-list-with-group navbox-list navbox-even hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Deuterium_fusion" title="Deuterium fusion">Deuterium fusion</a></li> <li><a href="/wiki/Lithium_burning" title="Lithium burning">Li burning</a></li> <li><a href="/wiki/Proton%E2%80%93proton_chain" title="Proton–proton chain">Proton–proton chain</a></li> <li><a class="mw-selflink selflink">CNO cycle</a></li> <li><a href="/wiki/Alpha_process" title="Alpha process">α process</a></li> <li><a href="/wiki/Triple-alpha_process" title="Triple-alpha process">Triple-α</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/R-process" title="R-process">r-process</a></li> <li><a href="/wiki/S-process" title="S-process">s-process</a></li> <li><a href="/wiki/P-process" title="P-process">p-process</a></li> <li><a href="/wiki/Rp-process" title="Rp-process">rp-process</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Other processes</th><td class="navbox-list-with-group navbox-list navbox-odd hlist" style="width:100%;padding:0"><div style="padding:0 0.25em"> <ul><li><a href="/wiki/Photodisintegration" title="Photodisintegration">Photodisintegration</a></li> <li><a href="/wiki/Photofission" title="Photofission">Photofission</a></li></ul> </div><table class="nowraplinks navbox-subgroup" style="border-spacing:0"><tbody><tr><th scope="row" class="navbox-group" style="width:1%">Capture</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/Neutron_capture" title="Neutron capture">Neutron capture</a></li> <li><a href="/wiki/Proton_capture" title="Proton capture">Proton capture</a></li></ul> </div></td></tr><tr><th scope="row" class="navbox-group" style="width:1%">Exchange</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/(n-p)_reaction" title="(n-p) reaction">(n-p) reaction</a></li></ul> </div></td></tr></tbody></table><div> </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 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