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The End of the Main Sequence - NASA/ADS
<!DOCTYPE html> <!--[if lt IE 7]> <html class="no-js lt-ie9 lt-ie8 lt-ie7"> <![endif]--> <!--[if IE 7]> <html class="no-js lt-ie9 lt-ie8"> <![endif]--> <!--[if IE 8]> <html class="no-js lt-ie9"> <![endif]--> <!--[if gt IE 8]><!--> <html class="no-js" lang="en"> <!--<![endif]--> <head> <title>The End of the Main Sequence - NASA/ADS</title> <!-- favicon --> <link rel="apple-touch-icon" sizes="180x180" href="//styles/favicon/apple-touch-icon.png" /> <link rel="icon" type="image/png" sizes="32x32" href="//styles/favicon/favicon-32x32.png" /> <link rel="icon" type="image/png" sizes="16x16" href="//styles/favicon/favicon-16x16.png" /> <link rel="manifest" href="//styles/favicon/site.webmanifest" /> <link rel="mask-icon" href="//styles/favicon/safari-pinned-tab.svg" color="#5bbad5" /> <meta name="apple-mobile-web-app-title" content="NASA ADS" /> <meta name="application-name" content="NASA ADS" /> <meta name="msapplication-TileColor" content="#ffc40d" /> <meta name="theme-color" content="#ffffff" /> <!-- /favicon --> <link rel="stylesheet" href="/styles/css/styles.css"> <meta name="robots" content="noarchive"> <link rel="canonical" href="http://ui.adsabs.harvard.edu/abs/1997ApJ...482..420L/abstract"/> <meta name="description" content="We present stellar evolution calculations for the lowest mass stars, i.e., those stars with masses in the range 0.08 M<SUB>⊙</SUB> &lt;= M<SUB>*</SUB> &lt;= 0.25 M<SUB>⊙</SUB>. Our particular emphasis is on the post-main-sequence evolution of these objects. We establish a hydrogen-burning timescale of τ<SUB>H</SUB> ~ 1.0 × 10<SUP>13</SUP> years for the minimum-mass main-sequence star. This timescale determines the duration over which the light of our Galaxy is dominated by a conventional stellar contribution. We find that for masses M<SUB>*</SUB> &lt; 0.25 M<SUB>⊙</SUB>, stars remain fully convective for a significant fraction of the duration of their evolution. The maintenance of full convection precludes the development of large composition gradients and allows the entire star to build up a large helium mass fraction. We find that stars with masses M &lt; 0.20 M<SUB>⊙</SUB> will never evolve through a red giant stage. After becoming gradually brighter and bluer for trillions of years, these late M dwarfs of today will develop radiative-conductive cores and mild nuclear shell sources; these stars then end their lives as helium white dwarfs. Our work has significant bearing on the general question of why stars become red giants. The fact that the lowest mass stars grow neither red nor giant as they evolve provides an important insight into this problem. Through both analytical and numerical arguments, we have determined that the development of low-mass red giants requires a combination of (1) increasing core luminosity, (2) the existence of molecular weight gradients between the core and the envelope, and (3) the presence of an atmospheric opacity which is an increasing function of temperature. Finally, we discuss the implications of our results with regards to the long-term fate and evolution of the Galaxy."> <!-- Open Graph --> <meta property="og:type" content="article"> <meta property="og:title" content="The End of the Main Sequence"> <meta property="og:site_name" content="NASA/ADS"> <meta property="og:description" content="We present stellar evolution calculations for the lowest mass stars, i.e., those stars with masses in the range 0.08 M<SUB>⊙</SUB> &lt;= M<SUB>*</SUB> &lt;= 0.25 M<SUB>⊙</SUB>. Our particular emphasis is on the post-main-sequence evolution of these objects. We establish a hydrogen-burning timescale of τ<SUB>H</SUB> ~ 1.0 × 10<SUP>13</SUP> years for the minimum-mass main-sequence star. This timescale determines the duration over which the light of our Galaxy is dominated by a conventional stellar contribution. We find that for masses M<SUB>*</SUB> &lt; 0.25 M<SUB>⊙</SUB>, stars remain fully convective for a significant fraction of the duration of their evolution. The maintenance of full convection precludes the development of large composition gradients and allows the entire star to build up a large helium mass fraction. We find that stars with masses M &lt; 0.20 M<SUB>⊙</SUB> will never evolve through a red giant stage. After becoming gradually brighter and bluer for trillions of years, these late M dwarfs of today will develop radiative-conductive cores and mild nuclear shell sources; these stars then end their lives as helium white dwarfs. Our work has significant bearing on the general question of why stars become red giants. The fact that the lowest mass stars grow neither red nor giant as they evolve provides an important insight into this problem. Through both analytical and numerical arguments, we have determined that the development of low-mass red giants requires a combination of (1) increasing core luminosity, (2) the existence of molecular weight gradients between the core and the envelope, and (3) the presence of an atmospheric opacity which is an increasing function of temperature. Finally, we discuss the implications of our results with regards to the long-term fate and evolution of the Galaxy."> <meta property="og:url" content="https://ui.adsabs.harvard.edu/abs/1997ApJ...482..420L/abstract"> <meta property="og:image" content="https://ui.adsabs.harvard.edu/styles/img/transparent_logo.svg"> <meta property="article:published_time" content="06/1997"> <meta property="article:author" content="Laughlin, Gregory"> <meta property="article:author" content="Bodenheimer, Peter"> <meta property="article:author" content="Adams, Fred C."> <!-- citation_* --> <meta name="citation_journal_title" content="The Astrophysical Journal"> <meta name="citation_authors" content="Laughlin, Gregory;Bodenheimer, Peter;Adams, Fred C."> <meta name="citation_title" content="The End of the Main Sequence"> <meta name="citation_date" content="06/1997"> <meta name="citation_volume" content="482"> <meta name="citation_issue" content="1"> <meta name="citation_firstpage" content="420"> <meta name="citation_doi" content="10.1086/304125"> <meta name="citation_issn" content="0004-637X"> <meta name="citation_language" content="en"> <meta name="citation_keywords" content="Stars: Evolution"> <meta name="citation_keywords" content="Stars: Interiors"> <meta name="citation_keywords" content="Stars: Late-Type"> <meta name="citation_keywords" content="Stars: Low-Mass"> <meta name="citation_keywords" content="Brown Dwarfs"> <meta name="citation_abstract_html_url" content="https://ui.adsabs.harvard.edu/abs/1997ApJ...482..420L/abstract"> <meta name="citation_publication_date" content="06/1997"> <meta name="citation_lastpage" content="432" /> <link title="schema(PRISM)" rel="schema.prism" href="http://prismstandard.org/namespaces/1.2/basic/" /> <meta name="prism.publicationDate" content="06/1997" /> <meta name="prism.publicationName" content="ApJ" /> <meta name="prism.issn" content="0004-637X" /> <meta name="prism.volume" content="482" /> <meta name="prism.startingPage" content="420" /> <meta name="prism.endingPage" content="432" /> <link title="schema(DC)" rel="schema.dc" href="http://purl.org/dc/elements/1.1/" /> <meta name="dc.identifier" content="doi:10.1086/304125" /> <meta name="dc.date" content="06/1997" /> <meta name="dc.source" content="ApJ" /> <meta name="dc.title" content="The End of the Main Sequence" /> <meta name="dc.creator" content="Laughlin, Gregory"> <meta name="dc.creator" content="Bodenheimer, Peter"> <meta name="dc.creator" content="Adams, Fred C."> <!-- twitter card --> <meta name="twitter:card" content="summary_large_image"/> <meta name="twitter:description" content="We present stellar evolution calculations for the lowest mass stars, i.e., those stars with masses in the range 0.08 M<SUB>⊙</SUB> &lt;= M<SUB>*</SUB> &lt;= 0.25 M<SUB>⊙</SUB>. Our particular emphasis is on the post-main-sequence evolution of these objects. We establish a hydrogen-burning timescale of τ<SUB>H</SUB> ~ 1.0 × 10<SUP>13</SUP> years for the minimum-mass main-sequence star. This timescale determines the duration over which the light of our Galaxy is dominated by a conventional stellar contribution. We find that for masses M<SUB>*</SUB> &lt; 0.25 M<SUB>⊙</SUB>, stars remain fully convective for a significant fraction of the duration of their evolution. The maintenance of full convection precludes the development of large composition gradients and allows the entire star to build up a large helium mass fraction. We find that stars with masses M &lt; 0.20 M<SUB>⊙</SUB> will never evolve through a red giant stage. After becoming gradually brighter and bluer for trillions of years, these late M dwarfs of today will develop radiative-conductive cores and mild nuclear shell sources; these stars then end their lives as helium white dwarfs. Our work has significant bearing on the general question of why stars become red giants. The fact that the lowest mass stars grow neither red nor giant as they evolve provides an important insight into this problem. Through both analytical and numerical arguments, we have determined that the development of low-mass red giants requires a combination of (1) increasing core luminosity, (2) the existence of molecular weight gradients between the core and the envelope, and (3) the presence of an atmospheric opacity which is an increasing function of temperature. Finally, we discuss the implications of our results with regards to the long-term fate and evolution of the Galaxy."/> <meta name="twitter:title" content="The End of the Main Sequence"/> <meta name="twitter:site" content="@adsabs"/> <meta name="twitter:domain" content="NASA/ADS"/> <meta name="twitter:image:src" content="https://ui.adsabs.harvard.edu/styles/img/transparent_logo.svg"/> <meta name="twitter:creator" content="@adsabs"/> <meta charset="utf-8"> <meta name="viewport" content="width=device-width, initial-scale=1, shrink-to-fit=no"> <base href="/"> <style> .btn-full-ads { color: #fff !important; background-color: #1a1a1a !important; border-color: #1a1a1a !important; margin-top: 9px !important; padding-bottom: 10px !important; padding-top: 10px !important; } .btn-full-ads:hover, .btn-full-ads:focus, .btn-full-ads:active, .btn-full-ads.active, .open>.dropdown-toggle.btn-full-ads { color: #000 !important; background-color: #ddd !important; border-color: #1a1a1a !important; } 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on the abstract page--> <div style="padding-left:4%"> <h4 class="s-list-description">Metrics for</h4> <h2 class="s-article-title"> The End of the Main Sequence </h2> </div> <div class="s-metrics-section" id="citations"> <div class="s-metrics-title"> <h3>Citations</h3> </div> <div class="metrics-table s-metrics-table"> <table class="table table-hover s-metrics-table table-condensed"> <thead> <tr> <th></th> <th></th> </tr> </thead> <tbody> <tr> <td> Total citations </td> <td> <i class="icon-help" title="The total number of times all papers in the list were cited."></i> </td> <td> 112 </td> </tr> <tr> <td> Normalized citations </td> <td> <i class="icon-help" title="For a list of N papers (i=1,...N), where Ni is the number of authors for publication i and Ci the number of citations that this paper received, the normalized citation count for each article is Ci/Ni, and the 'normalized citations' for this list of N papers is the sum of these N numbers."></i> </td> <td> 37.3 </td> </tr> <tr> <td> Refereed citations </td> <td> <i class="icon-help" title="Number of refereed citing papers."></i> </td> <td> 100 </td> </tr> <tr> <td> Normalized refereed citations </td> <td> <i class="icon-help" title="The normalized number of citations from refereed publications to all refereed publications in the list."></i> </td> <td> 33.3 </td> </tr> </tbody> </table> </div> <div class="metrics-graph s-metrics-graph"></div> </div> <div class="s-metrics-section" id="reads"> <div class="s-metrics-title"> <h3>Reads</h3> </div> <div class="metrics-table s-metrics-table"> <table class="table table-hover s-metrics-table table-condensed"> <thead> <tr> <th></th> <th></th> </tr> </thead> <tbody> <tr> <td> Total number of reads </td> <td> <i class="icon-help" title="The total number of times all papers were read. For each paper, a read is counted if an ADS user runs a search in our system and then requests to either view the paper's full bibliographic record or download the fulltext."></i> </td> <td> 4792 </td> </tr> <tr> <td> Total number of downloads </td> <td> <i class="icon-help" title="The total number of times full text (article or e-print) was accessed."></i> </td> <td> 1670 </td> </tr> </tbody> </table> </div> <div class="metrics-graph s-metrics-graph"></div> </div> </div> </div> </div> </div> </div> </div> <div class="s-right-col-container col-xs-12 col-sm-12 col-md-3 col-lg-2 s-right-column" id="right-col-container" > <div data-widget="ShowResources"> <div data-reactroot="" class="s-right-col-widget-container" style="padding: 10px" > <div> <div class="resources__container"> <div class="resources__full__list"> <div class="resources__header__row"> <i class="fa fa-file-text-o" aria-hidden="true"> </i> <div class="resources__header__title">full text sources</div> </div> <div class="resources__content"> <div class="resources__content__title">Publisher</div> <div class="resources__content__links"> <span> <div class="resources__content__link__separator">|</div> </span> <span> <a href="/link_gateway/1997ApJ...482..420L/PUB_HTML" rel="noopener" class="resources__content__link unlock" > <i class="fa fa-file-text" aria-hidden="true"> </i> </a> </span> </div> </div> </div> </div> <div data-widget="ShowAssociated"> </div> </div> </div> </div> <div data-widget="ShowGraphicsSidebar"> <div class="s-graphics-sidebar graphics-sidebar"> <div class="s-right-col-widget-container"> <div class="graphics-container s-graphics-container"> <h4 class="s-right-col-widget-title">Graphics</h4> <div class="grid-cell"> <a href="/abs/1997ApJ...482..420L/graphics" > <img src="https://s3.amazonaws.com/aasie/images/0004-637X/482/1/420/10_1086_304125_fg1_tb.gif" alt="figure from paper" class="grid-cell__image" /> <p><i>Click to view more</i></p> </a> </div> </div> </div> </div> </div> </div> <div class="col-lg-1"></div> </div> </div> </div> </div> </div> <div id="footer-container"> <div data-widget="FooterWidget"> <div class="footer s-footer"> <footer> <div class="__footer_wrapper"> <div class="__footer_brand"> © The SAO/NASA Astrophysics Data System <div class="__footer_brand_extra"> <p> <i class="fa fa-envelope"></i> adshelp[at]cfa.harvard.edu </p> <p> The ADS is operated by the Smithsonian Astrophysical Observatory under NASA Cooperative Agreement <em>NNX16AC86A</em> </p> </div> <div class="__footer_brand_logos"> <a href="http://www.nasa.gov" target="_blank" rel="noopener"> <img src="/styles/img/nasa.svg" alt="NASA logo" id="nasa-logo"> </a> <a href="http://www.si.edu" target="_blank" rel="noopener"> <img id="smithsonian-logo" src="/styles/img/smithsonian.svg" alt="Smithsonian logo"> </a> <a href="https://www.cfa.harvard.edu/" target="_blank" rel="noopener"> <img src="/styles/img/cfa.png" title="Harvard Center for Astrophysics logo" id="cfa-logo"> </a> </div> </div> <div class="__footer_list"> <div class="__footer_list_title"> Resources </div> <ul class="__footer_links"> <li> <a href="/about/" target="_blank" rel="noopener"> <i class="fa fa-question-circle"></i> About ADS </a> </li> <li> <a href="//ui.adsabs.harvard.edu/help/" target="_blank" rel="noopener"> <i class="fa fa-info-circle"></i> ADS Help </a> </li> <li> <a href="//ui.adsabs.harvard.edu/help/whats_new/" target="_blank" rel="noopener"> <i class="fa fa-bullhorn"></i> What's New </a> </li> <li> <a href="/about/careers/" target="_blank" rel="noopener"> <i class="fa fa-group"></i> Careers@ADS </a> </li> </ul> </div> <div class="__footer_list"> <div class="__footer_list_title"> Social </div> <ul class="__footer_links"> <li> <a href="//twitter.com/adsabs" target="_blank" rel="noopener"> <i class="fa fa-twitter"></i> @adsabs </a> </li> <li> <a href="//ui.adsabs.harvard.edu/blog/" target="_blank" rel="noopener"> <i class="fa fa-newspaper-o"></i> ADS Blog </a> </li> </ul> </div> <div class="__footer_list"> <div class="__footer_list_title"> Project </div> <ul class="__footer_links"> <li> <a href="/core/never">Switch to full ADS</a> </li> <li> <a href="https://adsisdownorjustme.herokuapp.com/" target="_blank" rel="noopener">Is ADS down? 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b.innerHTML += autoValues[i].match.substr(val.length); } // Insert a input field that will hold the current array item's value: b.innerHTML += "<input type='hidden' value='" + autoValues[i].value + "'>"; // Listen to clicks on the item value (DIV element): b.addEventListener("click", function(e) { var terms = searchBox.value.split(/\s+/); // Remove the current part of the input used for matching terms.pop(); // Insert the value for the autocomplete text field: terms.push(this.getElementsByTagName("input")[0].value); searchBox.value = terms.join(" "); // Move cursor position inside quotes/parenthesis if needed searchBox.focus(); if (searchBox.value[searchBox.value.length-1] === '"' || searchBox.value[searchBox.value.length-1] === ')') { searchBox.setSelectionRange(searchBox.value.length-1, searchBox.value.length-1); } // Close the list of autocompleted values closeAllLists(); }); a.appendChild(b); } } if (a.children.length > 0) { // By default, enter will select the first entry currentFocus = 0; 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// Add class "autocomplete-active": x[currentFocus].classList.add("autocomplete-active"); } function removeActive(x) { // Remove the "active" class from all autocomplete items: for (var i = 0; i < x.length; i++) { x[i].classList.remove("autocomplete-active"); } } function closeAllLists(elmnt) { // Close all autocomplete lists in the document, except the one passed as an argument: var x = document.getElementsByClassName("autocomplete-items"); for (var i = 0; i < x.length; i++) { if (elmnt != x[i] && elmnt != searchBox) { x[i].parentNode.removeChild(x[i]); } } } // Any other clicks in the document: document.addEventListener("click", function (e) { closeAllLists(e.target); }); } var autoList = [ { value: 'author:""', label: 'Author', match: 'author:"' }, { value: 'author:"^"', label: 'First Author', match: 'first author' }, { value: 'author:"^"', label: 'First Author', match: 'author:"^' }, { value: 'bibcode:""', label: 'Bibcode', desc: 'e.g. bibcode:1989ApJ...342L..71R', match: 'bibcode:"' }, { value: 'bibstem:""', label: 'Publication', desc: 'e.g. bibstem:ApJ', match: 'bibstem:"' }, { value: 'bibstem:""', label: 'Publication', desc: 'e.g. bibstem:ApJ', match: 'publication (bibstem)' }, { value: 'arXiv:', label: 'arXiv ID', match: 'arxiv:' }, { value: 'doi:', label: 'DOI', match: 'doi:' }, { value: 'full:""', label: 'Full text search', desc: 'title, abstract, and body', match: 'full:' }, { value: 'full:""', label: 'Full text search', desc: 'title, abstract, and body', match: 'fulltext' }, { value: 'full:""', label: 'Full text search', desc: 'title, abstract, and body', match: 'text' }, { value: 'year:', label: 'Year', match: 'year' }, { value: 'year:1999-2005', label: 'Year Range', desc: 'e.g. 1999-2005', match: 'year range' }, { value: 'aff:""', label: 'Affiliation', match: 'aff:' }, { value: 'abs:""', label: 'Search abstract + title + keywords', match: 'abs:' }, { value: 'database:astronomy', label: 'Limit to papers in the astronomy database', match: 'database:astronomy' }, { value: 'database:physics', label: 'Limit to papers in the physics database', match: 'database:physics' }, { value: 'title:""', label: 'Title', match: 'title:"' }, { value: 'orcid:', label: 'ORCiD identifier', match: 'orcid:' }, { value: 'object:', label: 'SIMBAD object (e.g. object:LMC)', match: 'object:' }, { value: 'property:refereed', label: 'Limit to refereed', desc: '(property:refereed)', match: 'refereed' }, { value: 'property:refereed', label: 'Limit to refereed', desc: '(property:refereed)', match: 'property:refereed' }, { value: 'property:notrefereed', label: 'Limit to non-refereed', desc: '(property:notrefereed)', match: 'property:notrefereed' }, { value: 'property:notrefereed', label: 'Limit to non-refereed', desc: '(property:notrefereed)', match: 'notrefereed' }, { value: 'property:eprint', label: 'Limit to eprints', desc: '(property:eprint)', match: 'eprint' }, { value: 'property:eprint', label: 'Limit to eprints', desc: '(property:eprint)', match: 'property:eprint' }, { value: 'property:openaccess', label: 'Limit to open access', desc: '(property:openaccess)', match: 'property:openaccess' }, { value: 'property:openaccess', label: 'Limit to open access', desc: '(property:openaccess)', match: 'openaccess' }, { value: 'doctype:software', label: 'Limit to software', desc: '(doctype:software)', match: 'software' }, { value: 'doctype:software', label: 'Limit to software', desc: '(doctype:software)', match: 'doctype:software' }, { value: 'property:inproceedings', label: 'Limit to papers in conference proceedings', desc: '(property:inproceedings)', match: 'proceedings' }, { value: 'property:inproceedings', label: 'Limit to papers in conference proceedings', desc: '(property:inproceedings)', match: 'property:inproceedings' }, { value: 'citations()', label: 'Citations', desc: 'Get papers citing your search result set', match: 'citations(' }, { value: 'references()', label: 'References', desc: 'Get papers referenced by your search result set', match: 'references(' }, { value: 'trending()', label: 'Trending', desc: 'Get papers most read by users who recently read your search result set', match: 'trending(' }, { value: 'reviews()', label: 'Review Articles', desc: 'Get most relevant papers that cite your search result set', match: 'reviews(' }, { value: 'useful()', label: 'Useful', desc: 'Get papers most frequently cited by your search result set', match: 'useful(' }, { value: 'similar()', label: 'Similar', desc: 'Get papers that have similar full text to your search result set', match: 'similar(' }, ]; 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