Search | arXiv e-print repository

<!DOCTYPE html> <html lang="en"> <head> <meta charset="utf-8"/> <meta name="viewport" content="width=device-width, initial-scale=1"/>  <link rel="apple-touch-icon" sizes="180x180" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/apple-touch-icon.png"> <link rel="icon" type="image/png" sizes="32x32" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/favicon-32x32.png"> <link rel="icon" type="image/png" sizes="16x16" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/favicon-16x16.png"> <link rel="manifest" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/site.webmanifest"> <link rel="mask-icon" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/safari-pinned-tab.svg" color="#b31b1b"> <link rel="shortcut icon" href="https://static.arxiv.org/static/base/1.0.0a5/images/icons/favicon.ico"> <meta name="msapplication-TileColor" content="#b31b1b"> <meta name="msapplication-config" content="images/icons/browserconfig.xml"> <meta name="theme-color" content="#b31b1b">  <title>Search | arXiv e-print repository</title> <script defer src="https://static.arxiv.org/static/base/1.0.0a5/fontawesome-free-5.11.2-web/js/all.js"></script> <link rel="stylesheet" href="https://static.arxiv.org/static/base/1.0.0a5/css/arxivstyle.css" /> <script type="text/x-mathjax-config"> MathJax.Hub.Config({ messageStyle: "none", extensions: ["tex2jax.js"], jax: ["input/TeX", "output/HTML-CSS"], tex2jax: { inlineMath: [ ['$','$'], ["\$","\$"] ], displayMath: [ ['$$','$$'], ["\\[","\\]"] ], processEscapes: true, ignoreClass: '.*', processClass: 'mathjax.*' }, TeX: { extensions: ["AMSmath.js", "AMSsymbols.js", "noErrors.js"], noErrors: { inlineDelimiters: ["$","$"], multiLine: false, style: { "font-size": "normal", "border": "" } } }, "HTML-CSS": { availableFonts: ["TeX"] } }); </script> <script src='//static.arxiv.org/MathJax-2.7.3/MathJax.js'></script> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/notification.js"></script> <link rel="stylesheet" href="https://static.arxiv.org/static/search/0.5.6/css/bulma-tooltip.min.css" /> <link rel="stylesheet" href="https://static.arxiv.org/static/search/0.5.6/css/search.css" /> <script src="https://code.jquery.com/jquery-3.2.1.slim.min.js" integrity="sha256-k2WSCIexGzOj3Euiig+TlR8gA0EmPjuc79OEeY5L45g=" crossorigin="anonymous"></script> <script src="https://static.arxiv.org/static/search/0.5.6/js/fieldset.js"></script> <style> radio#cf-customfield_11400 { display: none; } </style> </head> <body> <header><a href="#main-container" class="is-sr-only">Skip to main content</a>  <div class="attribution level is-marginless" role="banner"> <div class="level-left"> <a class="level-item" href="https://cornell.edu/"><img src="https://static.arxiv.org/static/base/1.0.0a5/images/cornell-reduced-white-SMALL.svg" alt="Cornell University" width="200" aria-label="logo" /></a> </div> <div class="level-right is-marginless"><p class="sponsors level-item is-marginless"><span id="support-ack-url">We gratefully acknowledge support from<br /> the Simons Foundation, <a href="https://info.arxiv.org/about/ourmembers.html">member institutions</a>, and all contributors. <a href="https://info.arxiv.org/about/donate.html">Donate</a></span></p></div> </div>  <div class="identity level is-marginless"> <div class="level-left"> <div class="level-item"> <a class="arxiv" href="https://arxiv.org/" aria-label="arxiv-logo"> <img src="https://static.arxiv.org/static/base/1.0.0a5/images/arxiv-logo-one-color-white.svg" aria-label="logo" alt="arxiv logo" width="85" style="width:85px;"/> </a> </div> </div> <div class="search-block level-right"> <form class="level-item mini-search" method="GET" action="https://arxiv.org/search"> <div class="field has-addons"> <div class="control"> <input class="input is-small" type="text" name="query" placeholder="Search..." aria-label="Search term or terms" /> <p class="help"><a href="https://info.arxiv.org/help">Help</a> | <a href="https://arxiv.org/search/advanced">Advanced Search</a></p> </div> <div class="control"> <div class="select is-small"> <select name="searchtype" aria-label="Field to search"> <option value="all" selected="selected">All fields</option> <option value="title">Title</option> <option value="author">Author</option> <option value="abstract">Abstract</option> <option value="comments">Comments</option> <option value="journal_ref">Journal reference</option> <option value="acm_class">ACM classification</option> <option value="msc_class">MSC classification</option> <option value="report_num">Report number</option> <option value="paper_id">arXiv identifier</option> <option value="doi">DOI</option> <option value="orcid">ORCID</option> <option value="author_id">arXiv author ID</option> <option value="help">Help pages</option> <option value="full_text">Full text</option> </select> </div> </div> <input type="hidden" name="source" value="header"> <button class="button is-small is-cul-darker">Search</button> </div> </form> </div> </div>  <div class="container"> <div class="user-tools is-size-7 has-text-right has-text-weight-bold" role="navigation" aria-label="User menu"> <a href="https://arxiv.org/login">Login</a> </div> </div> </header> <main class="container" id="main-container"> <div class="level is-marginless"> <div class="level-left"> <h1 class="title is-clearfix"> Showing 1–26 of 26 results for author: <span class="mathjax">Parikh, A</span> </h1> </div> <div class="level-right is-hidden-mobile">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> <div class="content"> <form method="GET" action="/search/nucl-ex" aria-role="search"> Searching in archive <strong>nucl-ex</strong>. <a href="/search/?searchtype=author&query=Parikh%2C+A">Search in all archives.</a> <div class="field has-addons-tablet"> <div class="control is-expanded"> <label for="query" class="hidden-label">Search term or terms</label> <input class="input is-medium" id="query" name="query" placeholder="Search term..." type="text" value="Parikh, A"> </div> <div class="select control is-medium"> <label class="is-hidden" for="searchtype">Field</label> <select class="is-medium" id="searchtype" name="searchtype"><option value="all">All fields</option><option value="title">Title</option><option selected value="author">Author(s)</option><option value="abstract">Abstract</option><option value="comments">Comments</option><option value="journal_ref">Journal reference</option><option value="acm_class">ACM classification</option><option value="msc_class">MSC classification</option><option value="report_num">Report number</option><option value="paper_id">arXiv identifier</option><option value="doi">DOI</option><option value="orcid">ORCID</option><option value="license">License (URI)</option><option value="author_id">arXiv author ID</option><option value="help">Help pages</option><option value="full_text">Full text</option></select> </div> <div class="control"> <button class="button is-link is-medium">Search</button> </div> </div> <div class="field"> <div class="control is-size-7"> <label class="radio"> <input checked id="abstracts-0" name="abstracts" type="radio" value="show"> Show abstracts </label> <label class="radio"> <input id="abstracts-1" name="abstracts" type="radio" value="hide"> Hide abstracts </label> </div> </div> <div class="is-clearfix" style="height: 2.5em"> <div class="is-pulled-right"> <a href="/search/advanced?terms-0-term=Parikh%2C+A&terms-0-field=author&size=50&order=-announced_date_first">Advanced Search</a> </div> </div> <input type="hidden" name="order" value="-announced_date_first"> <input type="hidden" name="size" value="50"> </form> <div class="level breathe-horizontal"> <div class="level-left"> <form method="GET" action="/search/"> <div style="display: none;"> <select id="searchtype" name="searchtype"><option value="all">All fields</option><option value="title">Title</option><option selected value="author">Author(s)</option><option value="abstract">Abstract</option><option value="comments">Comments</option><option value="journal_ref">Journal reference</option><option value="acm_class">ACM classification</option><option value="msc_class">MSC classification</option><option value="report_num">Report number</option><option value="paper_id">arXiv identifier</option><option value="doi">DOI</option><option value="orcid">ORCID</option><option value="license">License (URI)</option><option value="author_id">arXiv author ID</option><option value="help">Help pages</option><option value="full_text">Full text</option></select> <input id="query" name="query" type="text" value="Parikh, A"> <ul id="abstracts"><li><input checked id="abstracts-0" name="abstracts" type="radio" value="show"> <label for="abstracts-0">Show abstracts</label></li><li><input id="abstracts-1" name="abstracts" type="radio" value="hide"> <label for="abstracts-1">Hide abstracts</label></li></ul> </div> <div class="box field is-grouped is-grouped-multiline level-item"> <div class="control"> <span class="select is-small"> <select id="size" name="size"><option value="25">25</option><option selected value="50">50</option><option value="100">100</option><option value="200">200</option></select> </span> <label for="size">results per page</label>. </div> <div class="control"> <label for="order">Sort results by</label> <span class="select is-small"> <select id="order" name="order"><option selected value="-announced_date_first">Announcement date (newest first)</option><option value="announced_date_first">Announcement date (oldest first)</option><option value="-submitted_date">Submission date (newest first)</option><option value="submitted_date">Submission date (oldest first)</option><option value="">Relevance</option></select> </span> </div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.06472">arXiv:2209.06472</a> <span> [<a href="https://arxiv.org/pdf/2209.06472">pdf</a>, <a href="https://arxiv.org/format/2209.06472">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> First inverse kinematics measurement of resonances in $^7$Be($伪,纬$)$^{11}$C relevant to neutrino-driven wind nucleosynthesis using DRAGON </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Psaltis%2C+A">A. Psaltis</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+A+A">A. A. Chen</a>, <a href="/search/nucl-ex?searchtype=author&query=Longland%2C+R">R. Longland</a>, <a href="/search/nucl-ex?searchtype=author&query=Connolly%2C+D+S">D. S. Connolly</a>, <a href="/search/nucl-ex?searchtype=author&query=Brune%2C+C+R">C. R. Brune</a>, <a href="/search/nucl-ex?searchtype=author&query=Davids%2C+B">B. Davids</a>, <a href="/search/nucl-ex?searchtype=author&query=Fallis%2C+J">J. Fallis</a>, <a href="/search/nucl-ex?searchtype=author&query=Giri%2C+R">R. Giri</a>, <a href="/search/nucl-ex?searchtype=author&query=Greife%2C+U">U Greife</a>, <a href="/search/nucl-ex?searchtype=author&query=Hutcheon%2C+D+A">D. A. Hutcheon</a>, <a href="/search/nucl-ex?searchtype=author&query=Kroll%2C+L">L. Kroll</a>, <a href="/search/nucl-ex?searchtype=author&query=Lennarz%2C+A">A. Lennarz</a>, <a href="/search/nucl-ex?searchtype=author&query=Liang%2C+J">J. Liang</a>, <a href="/search/nucl-ex?searchtype=author&query=Lovely%2C+M">M. Lovely</a>, <a href="/search/nucl-ex?searchtype=author&query=Luo%2C+M">M. Luo</a>, <a href="/search/nucl-ex?searchtype=author&query=Marshall%2C+C">C. Marshall</a>, <a href="/search/nucl-ex?searchtype=author&query=Paneru%2C+S+N">S. N. Paneru</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Ruiz%2C+C">C. Ruiz</a>, <a href="/search/nucl-ex?searchtype=author&query=Shotter%2C+A+C">A. C. Shotter</a>, <a href="/search/nucl-ex?searchtype=author&query=Williams%2C+M">M. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.06472v1-abstract-short" style="display: inline;"> A possible mechanism to explain the origin of the light $p$-nuclei in the Galaxy is the nucleosynthesis in the proton-rich neutrino-driven wind ejecta of core-collapse supernovae via the $谓p$-process. However this production scenario is very sensitive to the underlying supernova dynamics and the nuclear physics input. As far as the nuclear uncertainties are concerned, the breakout from the $pp$-ch… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.06472v1-abstract-full').style.display = 'inline'; document.getElementById('2209.06472v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.06472v1-abstract-full" style="display: none;"> A possible mechanism to explain the origin of the light $p$-nuclei in the Galaxy is the nucleosynthesis in the proton-rich neutrino-driven wind ejecta of core-collapse supernovae via the $谓p$-process. However this production scenario is very sensitive to the underlying supernova dynamics and the nuclear physics input. As far as the nuclear uncertainties are concerned, the breakout from the $pp$-chains via the $^7$Be($伪,纬$)$^{11}$C reaction has been identified as an important link which can influence the nuclear flow and therefore the efficiency of the $谓p$-process. However its reaction rate is poorly known over the relevant temperature range, T = 1.5-3 GK. We report on the first direct measurement of two resonances of the $^7$Be($伪,纬$)$^{11}$C reaction with previously unknown strengths using an intense radioactive $^7$Be beam from the ISAC facility and the DRAGON recoil separator in inverse kinematics. We have decreased the $^7$Be($伪,纬$)$^{11}$C reaction rate uncertainty to $\sim$ 9.4-10.7% over the relevant temperature region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.06472v1-abstract-full').style.display = 'none'; document.getElementById('2209.06472v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 12 figures. Accepted for publication in Phys. Rev. C</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.06465">arXiv:2209.06465</a> <span> [<a href="https://arxiv.org/pdf/2209.06465">pdf</a>, <a href="https://arxiv.org/format/2209.06465">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Direct measurement of resonances in $^7$Be($伪,纬$)$^{11}$C relevant to $谓p$-process nucleosynthesis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Psaltis%2C+A">A. Psaltis</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+A+A">A. A. Chen</a>, <a href="/search/nucl-ex?searchtype=author&query=Longland%2C+R">R. Longland</a>, <a href="/search/nucl-ex?searchtype=author&query=Connolly%2C+D+S">D. S. Connolly</a>, <a href="/search/nucl-ex?searchtype=author&query=Brune%2C+C+R">C. R. Brune</a>, <a href="/search/nucl-ex?searchtype=author&query=Davids%2C+B">B. Davids</a>, <a href="/search/nucl-ex?searchtype=author&query=Fallis%2C+J">J. Fallis</a>, <a href="/search/nucl-ex?searchtype=author&query=Giri%2C+R">R. Giri</a>, <a href="/search/nucl-ex?searchtype=author&query=Greife%2C+U">U Greife</a>, <a href="/search/nucl-ex?searchtype=author&query=Hutcheon%2C+D+A">D. A. Hutcheon</a>, <a href="/search/nucl-ex?searchtype=author&query=Kroll%2C+L">L. Kroll</a>, <a href="/search/nucl-ex?searchtype=author&query=Lennarz%2C+A">A. Lennarz</a>, <a href="/search/nucl-ex?searchtype=author&query=Liang%2C+J">J. Liang</a>, <a href="/search/nucl-ex?searchtype=author&query=Lovely%2C+M">M. Lovely</a>, <a href="/search/nucl-ex?searchtype=author&query=Luo%2C+M">M. Luo</a>, <a href="/search/nucl-ex?searchtype=author&query=Marshall%2C+C">C. Marshall</a>, <a href="/search/nucl-ex?searchtype=author&query=Paneru%2C+S+N">S. N. Paneru</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Ruiz%2C+C">C. Ruiz</a>, <a href="/search/nucl-ex?searchtype=author&query=Shotter%2C+A+C">A. C. Shotter</a>, <a href="/search/nucl-ex?searchtype=author&query=Williams%2C+M">M. Williams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.06465v1-abstract-short" style="display: inline;"> We have performed the first direct measurement of two resonances of the $^7$Be($伪,纬$)$^{11}$C reaction with unknown strengths using an intense radioactive $^7$Be beam and the DRAGON recoil separator. We report on the first measurement of the 1155 and 1110 keV resonance strengths of $1.73 \pm 0.25(stat.) \pm 0.40(syst.)$ eV and $125 ^{+27}_{-25}(stat.) \pm 15(syst.)$ meV, respectively. The present… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.06465v1-abstract-full').style.display = 'inline'; document.getElementById('2209.06465v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.06465v1-abstract-full" style="display: none;"> We have performed the first direct measurement of two resonances of the $^7$Be($伪,纬$)$^{11}$C reaction with unknown strengths using an intense radioactive $^7$Be beam and the DRAGON recoil separator. We report on the first measurement of the 1155 and 1110 keV resonance strengths of $1.73 \pm 0.25(stat.) \pm 0.40(syst.)$ eV and $125 ^{+27}_{-25}(stat.) \pm 15(syst.)$ meV, respectively. The present results have reduced the uncertainty in the $^7$Be($伪,纬$)$^{11}$C reaction rate to $\sim$ 9.4-10.7% over T = 1.5-3 GK, which is relevant for nucleosynthesis in the neutrino-driven outflows of core-collapse supernovae ($谓p$-process). We find no effect of the new, constrained reaction rate on $谓p$-process nucleosynthesis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.06465v1-abstract-full').style.display = 'none'; document.getElementById('2209.06465v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 3 figures. Accepted for publication in Phys. Rev. Lett</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.09315">arXiv:2103.09315</a> <span> [<a href="https://arxiv.org/pdf/2103.09315">pdf</a>, <a href="https://arxiv.org/format/2103.09315">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/abee91">10.3847/1538-4357/abee91 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New experimental $^{23}$Na($伪,p$)$^{26}$Mg Reaction Rate for Massive Star and Type-Ia Supernova models </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Hubbard%2C+N+J">N. J. Hubbard</a>, <a href="/search/nucl-ex?searchtype=author&query=Diget%2C+C+A">C. Aa. Diget</a>, <a href="/search/nucl-ex?searchtype=author&query=Fox%2C+S+P">S. P. Fox</a>, <a href="/search/nucl-ex?searchtype=author&query=Fynbo%2C+H+O+U">H. O. U. Fynbo</a>, <a href="/search/nucl-ex?searchtype=author&query=Howard%2C+A+M">A. M. Howard</a>, <a href="/search/nucl-ex?searchtype=author&query=Kirsebom%2C+O+S">O. S. Kirsebom</a>, <a href="/search/nucl-ex?searchtype=author&query=Laird%2C+A+M">A. M. Laird</a>, <a href="/search/nucl-ex?searchtype=author&query=Munch%2C+M">M. Munch</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Pignatari%2C+M">M. Pignatari</a>, <a href="/search/nucl-ex?searchtype=author&query=Tomlinson%2C+J+R">J. R. Tomlinson</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2103.09315v1-abstract-short" style="display: inline;"> The $^{23}$Na($伪,p$)$^{26}$Mg reaction has been identified as having a significant impact on the nucleosynthesis of several nuclei between Ne and Ti in type-Ia supernovae, and of $^{23}$Na and $^{26}$Al in massive stars. The reaction has been subjected to renewed experimental interest recently, motivated by high uncertainties in early experimental data and in the statistical Hauser-Feshbach models… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.09315v1-abstract-full').style.display = 'inline'; document.getElementById('2103.09315v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.09315v1-abstract-full" style="display: none;"> The $^{23}$Na($伪,p$)$^{26}$Mg reaction has been identified as having a significant impact on the nucleosynthesis of several nuclei between Ne and Ti in type-Ia supernovae, and of $^{23}$Na and $^{26}$Al in massive stars. The reaction has been subjected to renewed experimental interest recently, motivated by high uncertainties in early experimental data and in the statistical Hauser-Feshbach models used in reaction rate compilations. Early experiments were affected by target deterioration issues and unquantifiable uncertainties. Three new independent measurements instead are utilizing inverse kinematics and Rutherford scattering monitoring to resolve this. In this work we present directly measured angular distributions of the emitted protons to eliminate a discrepancy in the assumptions made in the recent reaction rate measurements, which results in cross sections differing by a factor of 3. We derive a new combined experimental reaction rate for the $^{23}$Na($伪,p$)$^{26}$Mg reaction with a total uncertainty of 30% at relevant temperatures. Using our new $^{23}$Na($伪,p$)$^{26}$Mg rate, the $^{26}$Al and $^{23}$Na production uncertainty is reduced to within 8%. In comparison, using the factor of 10 uncertainty previously recommended by the rate compilation STARLIB, $^{26}$Al and $^{23}$Na production was changing by more than a factor of 2. In type-Ia supernova conditions, the impact on production of $^{23}$Na is constrained to within 15%. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.09315v1-abstract-full').style.display = 'none'; document.getElementById('2103.09315v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 8 figures, 4 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 912 59 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.13222">arXiv:2011.13222</a> <span> [<a href="https://arxiv.org/pdf/2011.13222">pdf</a>, <a href="https://arxiv.org/format/2011.13222">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.103.015807">10.1103/PhysRevC.103.015807 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sub-threshold states in $^{19}$Ne relevant to $^{18}$F(p,$伪$)$^{15}$O </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Riley%2C+J+E">J. E. Riley</a>, <a href="/search/nucl-ex?searchtype=author&query=Laird%2C+A+M">A. M. Laird</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Fox%2C+S+P">S. P. Fox</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Stefan%2C+I">I. Stefan</a>, <a href="/search/nucl-ex?searchtype=author&query=Adsley%2C+P">P. Adsley</a>, <a href="/search/nucl-ex?searchtype=author&query=Assi%C3%A9%2C+M">M. Assi茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Bastin%2C+B">B. Bastin</a>, <a href="/search/nucl-ex?searchtype=author&query=Boulay%2C+F">F. Boulay</a>, <a href="/search/nucl-ex?searchtype=author&query=Coc%2C+A">A. Coc</a>, <a href="/search/nucl-ex?searchtype=author&query=Franchoo%2C+S">S. Franchoo</a>, <a href="/search/nucl-ex?searchtype=author&query=Garg%2C+R">R. Garg</a>, <a href="/search/nucl-ex?searchtype=author&query=Gillespie%2C+S+A">S. A. Gillespie</a>, <a href="/search/nucl-ex?searchtype=author&query=Guimaraes%2C+V">V. Guimaraes</a>, <a href="/search/nucl-ex?searchtype=author&query=Hamadache%2C+C">C. Hamadache</a>, <a href="/search/nucl-ex?searchtype=author&query=Hubbard%2C+N">N. Hubbard</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Lefebvre-Schuhl%2C+A">A. Lefebvre-Schuhl</a>, <a href="/search/nucl-ex?searchtype=author&query=Santos%2C+F+d+O">F. de Oliveira Santos</a>, <a href="/search/nucl-ex?searchtype=author&query=Remadi%2C+A">A. Remadi</a>, <a href="/search/nucl-ex?searchtype=author&query=Perrot%2C+L">L. Perrot</a>, <a href="/search/nucl-ex?searchtype=author&query=Suzuki%2C+D">D. Suzuki</a>, <a href="/search/nucl-ex?searchtype=author&query=Verde%2C+G">G. Verde</a> , et al. (2 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2011.13222v1-abstract-short" style="display: inline;"> Classical novae result from thermonuclear explosions producing several $纬$-ray emitters which are prime targets for satellites observing in the MeV range. The early 511 keV gamma-ray emission depends critically on the $^{18}$F(p,$伪$)$^{15}$O reaction rate which, despite many experimental and theoretical efforts, still remains uncertain. One of the main uncertainties in the $^{18}$F(p,$伪$)$^{15}$O… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.13222v1-abstract-full').style.display = 'inline'; document.getElementById('2011.13222v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.13222v1-abstract-full" style="display: none;"> Classical novae result from thermonuclear explosions producing several $纬$-ray emitters which are prime targets for satellites observing in the MeV range. The early 511 keV gamma-ray emission depends critically on the $^{18}$F(p,$伪$)$^{15}$O reaction rate which, despite many experimental and theoretical efforts, still remains uncertain. One of the main uncertainties in the $^{18}$F(p,$伪$)$^{15}$O reaction rate is the contribution in the Gamow window of interference between sub-threshold $^{19}$Ne states and known broad states at higher energies. Therefore the goal of this work is to clarify the existence and the nature of these sub-threshold states. States in the $^{19}$Ne compound nucleus were studied at the Tandem-ALTO facility using the $^{19}$F($^3$He,t)$^{19}$Ne charge exchange reaction. Tritons were detected with an Enge Split-pole spectrometer while decaying protons or $伪$-particles from unbound $^{19}$Ne states were collected, in coincidence, with a double-sided silicon strip detector array. Angular correlations were extracted and constraints on the spin and parity of decaying states established. The coincidence yield at $E_x$ = 6.29 MeV was observed to be high spin, supporting the conclusion that it is indeed a doublet consisting of high spin and low spin components. Evidence for a broad, low spin state was observed around 6 MeV. Branching ratios were extracted for several states above the proton threshold and were found to be consistent with the literature. R-matrix calculations show the relative contribution of sub-threshold states to the astrophysically important energy region above the proton threshold. The levels schemes of $^{19}$Ne and $^{19}$F are still not sufficiently well known and further studies of the analogue assignments are needed. The tentative broad state at 6 MeV may only play a role if the reduced proton width is large. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.13222v1-abstract-full').style.display = 'none'; document.getElementById('2011.13222v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1701.03088">arXiv:1701.03088</a> <span> [<a href="https://arxiv.org/pdf/1701.03088">pdf</a>, <a href="https://arxiv.org/ps/1701.03088">ps</a>, <a href="https://arxiv.org/format/1701.03088">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.97.015802">10.1103/PhysRevC.97.015802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First measurement of $^{30}$S+$伪$ resonant elastic scattering for the $^{30}$S($伪$,p) reaction rate </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Kahl%2C+D">D. Kahl</a>, <a href="/search/nucl-ex?searchtype=author&query=Yamaguchi%2C+H">H. Yamaguchi</a>, <a href="/search/nucl-ex?searchtype=author&query=Kubono%2C+S">S. Kubono</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+A+A">A. A. Chen</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Binh%2C+D+N">D. N. Binh</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+J">J. Chen</a>, <a href="/search/nucl-ex?searchtype=author&query=Cherubini%2C+S">S. Cherubini</a>, <a href="/search/nucl-ex?searchtype=author&query=Duy%2C+N+N">N. N. Duy</a>, <a href="/search/nucl-ex?searchtype=author&query=Hashimoto%2C+T">T. Hashimoto</a>, <a href="/search/nucl-ex?searchtype=author&query=Hayakawa%2C+S">S. Hayakawa</a>, <a href="/search/nucl-ex?searchtype=author&query=Iwasa%2C+N">N. Iwasa</a>, <a href="/search/nucl-ex?searchtype=author&query=Jung%2C+H+S">H. S. Jung</a>, <a href="/search/nucl-ex?searchtype=author&query=Kato%2C+S">S. Kato</a>, <a href="/search/nucl-ex?searchtype=author&query=Kwon%2C+Y+K">Y. K. Kwon</a>, <a href="/search/nucl-ex?searchtype=author&query=Nishimura%2C+S">S. Nishimura</a>, <a href="/search/nucl-ex?searchtype=author&query=Ota%2C+S">S. Ota</a>, <a href="/search/nucl-ex?searchtype=author&query=Setoodehnia%2C+K">K. Setoodehnia</a>, <a href="/search/nucl-ex?searchtype=author&query=Teranishi%2C+T">T. Teranishi</a>, <a href="/search/nucl-ex?searchtype=author&query=Tokieda%2C+H">H. Tokieda</a>, <a href="/search/nucl-ex?searchtype=author&query=Yamada%2C+T">T. Yamada</a>, <a href="/search/nucl-ex?searchtype=author&query=Yun%2C+C+C">C. C. Yun</a>, <a href="/search/nucl-ex?searchtype=author&query=Zhang%2C+L+Y">L. Y. Zhang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1701.03088v3-abstract-short" style="display: inline;"> Background: Type I x-ray bursts are the most frequent thermonuclear explosions in the galaxy, resulting from thermonuclear runaway on the surface of an accreting neutron star. The $^{30}$S($伪$,p) reaction plays a critical role in burst models, yet insufficient experimental information is available to calculate a reliable, precise rate for this reaction. Purpose: Our measurement was conducted to se… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.03088v3-abstract-full').style.display = 'inline'; document.getElementById('1701.03088v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1701.03088v3-abstract-full" style="display: none;"> Background: Type I x-ray bursts are the most frequent thermonuclear explosions in the galaxy, resulting from thermonuclear runaway on the surface of an accreting neutron star. The $^{30}$S($伪$,p) reaction plays a critical role in burst models, yet insufficient experimental information is available to calculate a reliable, precise rate for this reaction. Purpose: Our measurement was conducted to search for states in $^{34}$Ar and determine their quantum properties. In particular, natural-parity states with large $伪$-decay partial widths should dominate the stellar reaction rate. Method: We performed the first measurement of $^{30}$S+$伪$ resonant elastic scattering up to a center-of-mass energy of 5.5 MeV using a radioactive ion beam. The experiment utilized a thick gaseous active target system and silicon detector array in inverse kinematics. Results: We obtained an excitation function for $^{30}$S($伪$,$伪$) near $150^{\circ}$ in the center-of-mass frame. The experimental data were analyzed with an $R$-Matrix calculation, and we observed three new resonant patterns between 11.1 and 12.1 MeV, extracting their properties of resonance energy, widths, spin, and parity. Conclusions: We calculated the resonant thermonuclear reaction rate of $^{30}$S($伪$,p) based on all available experimental data of $^{34}$Ar and found an upper limit about one order of magnitude larger than a rate determined using a statistical model. The astrophysical impact of these two rates has been investigated through one-zone postprocessing type I x-ray burst calculations. We find that our new upper limit for the $^{30}$S($伪$,p)$^{33}$Cl rate significantly affects the predicted nuclear energy generation rate during the burst. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1701.03088v3-abstract-full').style.display = 'none'; document.getElementById('1701.03088v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 January, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 97, 015802 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.00901">arXiv:1511.00901</a> <span> [<a href="https://arxiv.org/pdf/1511.00901">pdf</a>, <a href="https://arxiv.org/ps/1511.00901">ps</a>, <a href="https://arxiv.org/format/1511.00901">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.92.055806">10.1103/PhysRevC.92.055806 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectroscopy of $^{19}$Ne for the thermonuclear $^{15}$O($伪,纬$)$^{19}$Ne and $^{18}$F($p,伪$)$^{15}$O reaction rates </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Laird%2C+A+M">A. M. Laird</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Wimmer%2C+K">K. Wimmer</a>, <a href="/search/nucl-ex?searchtype=author&query=Faestermann%2C+T">T. Faestermann</a>, <a href="/search/nucl-ex?searchtype=author&query=Hertenberger%2C+R">R. Hertenberger</a>, <a href="/search/nucl-ex?searchtype=author&query=Seiler%2C+D">D. Seiler</a>, <a href="/search/nucl-ex?searchtype=author&query=Wirth%2C+H+-">H. -F. Wirth</a>, <a href="/search/nucl-ex?searchtype=author&query=Adsley%2C+P">P. Adsley</a>, <a href="/search/nucl-ex?searchtype=author&query=Fulton%2C+B+R">B. R. Fulton</a>, <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Stefan%2C+I">I. Stefan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1511.00901v1-abstract-short" style="display: inline;"> Uncertainties in the thermonuclear rates of the $^{15}$O($伪,纬$)$^{19}$Ne and $^{18}$F($p,伪$)$^{15}$O reactions affect model predictions of light curves from type I X-ray bursts and the amount of the observable radioisotope $^{18}$F produced in classical novae, respectively. To address these uncertainties, we have studied the nuclear structure of $^{19}$Ne over $E_{x} = 4.0 - 5.1$ MeV and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.00901v1-abstract-full').style.display = 'inline'; document.getElementById('1511.00901v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.00901v1-abstract-full" style="display: none;"> Uncertainties in the thermonuclear rates of the $^{15}$O($伪,纬$)$^{19}$Ne and $^{18}$F($p,伪$)$^{15}$O reactions affect model predictions of light curves from type I X-ray bursts and the amount of the observable radioisotope $^{18}$F produced in classical novae, respectively. To address these uncertainties, we have studied the nuclear structure of $^{19}$Ne over $E_{x} = 4.0 - 5.1$ MeV and $6.1 - 7.3$ MeV using the $^{19}$F($^{3}$He,t)$^{19}$Ne reaction. We find the $J^蟺$ values of the 4.14 and 4.20 MeV levels to be consistent with $9/2^{-}$ and $7/2^{-}$ respectively, in contrast to previous assumptions. We confirm the recently observed triplet of states around 6.4 MeV, and find evidence that the state at 6.29 MeV, just below the proton threshold, is either broad or a doublet. Our data also suggest that predicted but yet unobserved levels may exist near the 6.86 MeV state. Higher resolution experiments are urgently needed to further clarify the structure of $^{19}$Ne around the proton threshold before a reliable $^{18}$F($p,伪$)$^{15}$O rate for nova models can be determined. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.00901v1-abstract-full').style.display = 'none'; document.getElementById('1511.00901v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 3 figures, Phys. Rev. C (in press)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1510.04313">arXiv:1510.04313</a> <span> [<a href="https://arxiv.org/pdf/1510.04313">pdf</a>, <a href="https://arxiv.org/format/1510.04313">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.91.015803">10.1103/PhysRevC.91.015803 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Discovery of $^{34g,m}$Cl$(p,纬)^{35}$Ar resonances activated at classical nova temperatures </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Fry%2C+C">C. Fry</a>, <a href="/search/nucl-ex?searchtype=author&query=Wrede%2C+C">C. Wrede</a>, <a href="/search/nucl-ex?searchtype=author&query=Bishop%2C+S">S. Bishop</a>, <a href="/search/nucl-ex?searchtype=author&query=Brown%2C+B+A">B. A. Brown</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+A+A">A. A. Chen</a>, <a href="/search/nucl-ex?searchtype=author&query=Faestermann%2C+T">T. Faestermann</a>, <a href="/search/nucl-ex?searchtype=author&query=Hertenberger%2C+R">R. Hertenberger</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=P%C3%A9rez-Loureiro%2C+D">D. P茅rez-Loureiro</a>, <a href="/search/nucl-ex?searchtype=author&query=Wirth%2C+H+-">H. -F. Wirth</a>, <a href="/search/nucl-ex?searchtype=author&query=Garc%C3%ADa%2C+A">A. Garc铆a</a>, <a href="/search/nucl-ex?searchtype=author&query=Ortez%2C+R">R. Ortez</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1510.04313v1-abstract-short" style="display: inline;"> Background: The thermonuclear $^{34g,m}$Cl($p,纬$)$^{35}$Ar reaction rates are unknown due to a lack of experimental nuclear physics data. Uncertainties in these rates translate to uncertainties in $^{34}$S production in models of classical novae on oxygen-neon white dwarfs. $^{34}$S abundances have the potential to aid in the classification of presolar grains. Purpose: Determine resonance energi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.04313v1-abstract-full').style.display = 'inline'; document.getElementById('1510.04313v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1510.04313v1-abstract-full" style="display: none;"> Background: The thermonuclear $^{34g,m}$Cl($p,纬$)$^{35}$Ar reaction rates are unknown due to a lack of experimental nuclear physics data. Uncertainties in these rates translate to uncertainties in $^{34}$S production in models of classical novae on oxygen-neon white dwarfs. $^{34}$S abundances have the potential to aid in the classification of presolar grains. Purpose: Determine resonance energies for the $^{34g,m}$Cl($p,纬$)$^{35}$Ar reactions within the region of astrophyical interest for classical novae to a precision of a few keV as an essential first step toward constraining their thermonuclear reaction rates. Method: $^{35}$Ar excited states were populated by the $^{36}$Ar($d,t$)$^{35}$Ar reaction at $E$(d)=22~MeV and reaction products were momentum analyzed by a high resolution quadrupole-dipole-dipole-dipole (Q3D) magnetic spectrograph. Results: Seventeen new $^{35}$Ar levels have been detected at a statistically significant level in the region $E_x\approx$~5.9-6.7~MeV ($E_r$ \textless~800~ keV) and their excitation energies have been determined to typical uncertainties of 3~keV. The uncertainties for five previously known levels have also been reduced substantially. The measured level density was compared to those calculated using the WBMB Hamiltonian within the $sd-pf$ model space. Conclusions: Most of the resonances in the region of astrophyical interest have likely been discovered and their energies have been determined, but the resonance strengths are still unknown, and experimentally constraining the $^{34g,m}$Cl($p,纬$)$^{35}$Ar reaction rates will require further experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.04313v1-abstract-full').style.display = 'none'; document.getElementById('1510.04313v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 October, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 3 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. C 91, 015803 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1409.0326">arXiv:1409.0326</a> <span> [<a href="https://arxiv.org/pdf/1409.0326">pdf</a>, <a href="https://arxiv.org/ps/1409.0326">ps</a>, <a href="https://arxiv.org/format/1409.0326">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.physletb.2014.08.071">10.1016/j.physletb.2014.08.071 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Isotopic 32S/33S ratio as a diagnostic of presolar grains from novae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Wimmer%2C+K">K. Wimmer</a>, <a href="/search/nucl-ex?searchtype=author&query=Faestermann%2C+T">T. Faestermann</a>, <a href="/search/nucl-ex?searchtype=author&query=Hertenberger%2C+R">R. Hertenberger</a>, <a href="/search/nucl-ex?searchtype=author&query=Jose%2C+J">J. Jose</a>, <a href="/search/nucl-ex?searchtype=author&query=Wirth%2C+H+-">H. -F. Wirth</a>, <a href="/search/nucl-ex?searchtype=author&query=Hinke%2C+C">C. Hinke</a>, <a href="/search/nucl-ex?searchtype=author&query=Krucken%2C+R">R. Krucken</a>, <a href="/search/nucl-ex?searchtype=author&query=Seiler%2C+D">D. Seiler</a>, <a href="/search/nucl-ex?searchtype=author&query=Steiger%2C+K">K. Steiger</a>, <a href="/search/nucl-ex?searchtype=author&query=Straub%2C+K">K. Straub</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1409.0326v1-abstract-short" style="display: inline;"> Measurements of sulphur isotopes in presolar grains can help to identify the astrophysical sites in which these grains were formed. A more precise thermonuclear rate of the 33S(p,gamma)34Cl reaction is required, however, to assess the diagnostic ability of sulphur isotopic ratios. We have studied the 33S(3He,d)34Cl proton-transfer reaction at 25 MeV using a high-resolution quadrupole-dipole-dipole… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.0326v1-abstract-full').style.display = 'inline'; document.getElementById('1409.0326v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1409.0326v1-abstract-full" style="display: none;"> Measurements of sulphur isotopes in presolar grains can help to identify the astrophysical sites in which these grains were formed. A more precise thermonuclear rate of the 33S(p,gamma)34Cl reaction is required, however, to assess the diagnostic ability of sulphur isotopic ratios. We have studied the 33S(3He,d)34Cl proton-transfer reaction at 25 MeV using a high-resolution quadrupole-dipole-dipole-dipole magnetic spectrograph. Deuteron spectra were measured at ten scattering angles between 10 and 55 degrees. Twenty-four levels in 34Cl over Ex = 4.6 - 5.9 MeV were observed, including three levels for the first time. Proton spectroscopic factors were extracted for the first time for levels above the 33S+p threshold, spanning the energy range required for calculations of the thermonuclear 33S(p,gamma)34Cl rate in classical nova explosions. We have determined a new 33S(p,gamma)34Cl rate using a Monte Carlo method and have performed new hydrodynamic nova simulations to determine the impact on nova nucleosynthesis of remaining nuclear physics uncertainties in the reaction rate. We find that these uncertainties lead to a factor of less than 5 variation in the 33S(p,gamma)34Cl rate over typical nova peak temperatures, and variation in the ejected nova yields of S--Ca isotopes by less than 20%. In particular, the predicted 32S/33S ratio is 110 - 130 for the nova model considered, compared to 110 - 440 with previous rate uncertainties. As recent type II supernova models predict ratios of 130 - 200, the 32S/33S ratio may be used to distinguish between grains of nova and supernova origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.0326v1-abstract-full').style.display = 'none'; document.getElementById('1409.0326v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 September, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 3 figures, 3 tables, Phys. Lett. B (in press)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Lett. B 737, 314 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1407.4246">arXiv:1407.4246</a> <span> [<a href="https://arxiv.org/pdf/1407.4246">pdf</a>, <a href="https://arxiv.org/ps/1407.4246">ps</a>, <a href="https://arxiv.org/format/1407.4246">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.90.025803">10.1103/PhysRevC.90.025803 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Examination of the role of the $^{14}$O($伪$,$p$)$^{17}$F reaction rate in type I x-ray bursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Hu%2C+J">J. Hu</a>, <a href="/search/nucl-ex?searchtype=author&query=He%2C+J+J">J. J. He</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Xu%2C+S+W">S. W. Xu</a>, <a href="/search/nucl-ex?searchtype=author&query=Yamaguchi%2C+H">H. Yamaguchi</a>, <a href="/search/nucl-ex?searchtype=author&query=Kahl%2C+D">D. Kahl</a>, <a href="/search/nucl-ex?searchtype=author&query=Ma%2C+P">P. Ma</a>, <a href="/search/nucl-ex?searchtype=author&query=Su%2C+J">J. Su</a>, <a href="/search/nucl-ex?searchtype=author&query=Wang%2C+H+W">H. W. Wang</a>, <a href="/search/nucl-ex?searchtype=author&query=Nakao%2C+T">T. Nakao</a>, <a href="/search/nucl-ex?searchtype=author&query=Wakabayashi%2C+Y">Y. Wakabayashi</a>, <a href="/search/nucl-ex?searchtype=author&query=Teranishi%2C+T">T. Teranishi</a>, <a href="/search/nucl-ex?searchtype=author&query=Hahn%2C+K+I">K. I. Hahn</a>, <a href="/search/nucl-ex?searchtype=author&query=Moon%2C+J+Y">J. Y. Moon</a>, <a href="/search/nucl-ex?searchtype=author&query=Jung%2C+H+S">H. S. Jung</a>, <a href="/search/nucl-ex?searchtype=author&query=Hashimoto%2C+T">T. Hashimoto</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+A+A">A. A. Chen</a>, <a href="/search/nucl-ex?searchtype=author&query=Irvine%2C+D">D. Irvine</a>, <a href="/search/nucl-ex?searchtype=author&query=Lee%2C+C+S">C. S. Lee</a>, <a href="/search/nucl-ex?searchtype=author&query=Kubono%2C+S">S. Kubono</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1407.4246v1-abstract-short" style="display: inline;"> The $^{14}$O($伪$,$p$)$^{17}$F reaction is one of the key reactions involved in the breakout from the hot-CNO cycle to the rp-process in type I x-ray bursts (XRBs). The resonant properties in the compound nucleus $^{18}$Ne have been investigated through resonant elastic scattering of $^{17}$F+$p$. The radioactive $^{17}$F beam was separated by the CNS Radioactive Ion Beam separator (CRIB) and bomba… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.4246v1-abstract-full').style.display = 'inline'; document.getElementById('1407.4246v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1407.4246v1-abstract-full" style="display: none;"> The $^{14}$O($伪$,$p$)$^{17}$F reaction is one of the key reactions involved in the breakout from the hot-CNO cycle to the rp-process in type I x-ray bursts (XRBs). The resonant properties in the compound nucleus $^{18}$Ne have been investigated through resonant elastic scattering of $^{17}$F+$p$. The radioactive $^{17}$F beam was separated by the CNS Radioactive Ion Beam separator (CRIB) and bombarded a thick H$_2$ gas target at 3.6 MeV/nucleon. The recoiling light particles were measured by three $螖$E-E silicon telescopes at laboratory angles of $胃$$_{lab}$$\approx$3$^\circ$, 10$^\circ$ and 18$^\circ$, respectively. Five resonances at $E_{x}$=6.15, 6.28, 6.35, 6.85, and 7.05 MeV were observed in the excitation functions, and their spin-parities have been determined based on an $R$-matrix analysis. In particular, $J^蟺$=1$^-$ was firmly assigned to the 6.15-MeV state which dominates the thermonuclear $^{14}$O($伪$,$p$)$^{17}$F rate below 2 GK. As well, a possible new excited state in $^{18}$Ne was observed at $E_{x}$=6.85$\pm$0.11 MeV with tentative $J$=0 assignment. This state could be the analog state of the 6.880 MeV (0$^{-}$) level in the mirror nucleus $^{18}$O, or a bandhead state (0$^+$) of the six-particle four-hole (6$p$-4$h$) band. A new thermonuclear $^{14}$O($伪$,$p$)$^{17}$F rate has been determined, and the astrophysical impact of multiple recent rates has been examined using an XRB model. Contrary to previous expectations, we find only modest impact on predicted nuclear energy generation rates from using reaction rates differing by up to several orders of magnitude. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.4246v1-abstract-full').style.display = 'none'; document.getElementById('1407.4246v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 July, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 5 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1403.4668">arXiv:1403.4668</a> <span> [<a href="https://arxiv.org/pdf/1403.4668">pdf</a>, <a href="https://arxiv.org/ps/1403.4668">ps</a>, <a href="https://arxiv.org/format/1403.4668">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.89.015804">10.1103/PhysRevC.89.015804 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Investigation of thermonuclear $^{18}$Ne($伪$,$p$)$^{21}$Na rate via resonant elastic scattering of $^{21}$Na+$p$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Zhang%2C+L+Y">L. Y. Zhang</a>, <a href="/search/nucl-ex?searchtype=author&query=He%2C+J+J">J. J. He</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Xu%2C+S+W">S. W. Xu</a>, <a href="/search/nucl-ex?searchtype=author&query=Yamaguchi%2C+H">H. Yamaguchi</a>, <a href="/search/nucl-ex?searchtype=author&query=Kahl%2C+D">D. Kahl</a>, <a href="/search/nucl-ex?searchtype=author&query=Kubono%2C+S">S. Kubono</a>, <a href="/search/nucl-ex?searchtype=author&query=Mohr%2C+P">P. Mohr</a>, <a href="/search/nucl-ex?searchtype=author&query=Hu%2C+J">J. Hu</a>, <a href="/search/nucl-ex?searchtype=author&query=Ma%2C+P">P. Ma</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+S+Z">S. Z. Chen</a>, <a href="/search/nucl-ex?searchtype=author&query=Wakabayashi%2C+Y">Y. Wakabayashi</a>, <a href="/search/nucl-ex?searchtype=author&query=Wang%2C+H+W">H. W. Wang</a>, <a href="/search/nucl-ex?searchtype=author&query=Tian%2C+W+D">W. D. Tian</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+R+F">R. F. Chen</a>, <a href="/search/nucl-ex?searchtype=author&query=Guo%2C+B">B. Guo</a>, <a href="/search/nucl-ex?searchtype=author&query=Hashimoto%2C+T">T. Hashimoto</a>, <a href="/search/nucl-ex?searchtype=author&query=Togano%2C+Y">Y. Togano</a>, <a href="/search/nucl-ex?searchtype=author&query=Hayakawa%2C+S">S. Hayakawa</a>, <a href="/search/nucl-ex?searchtype=author&query=Teranishi%2C+T">T. Teranishi</a>, <a href="/search/nucl-ex?searchtype=author&query=Iwasa%2C+N">N. Iwasa</a>, <a href="/search/nucl-ex?searchtype=author&query=Yamada%2C+T">T. Yamada</a>, <a href="/search/nucl-ex?searchtype=author&query=Komatsubara%2C+T">T. Komatsubara</a>, <a href="/search/nucl-ex?searchtype=author&query=Zhang%2C+Y+H">Y. H. Zhang</a>, <a href="/search/nucl-ex?searchtype=author&query=Zhou%2C+X+H">X. H. Zhou</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1403.4668v1-abstract-short" style="display: inline;"> The $^{18}$Ne($伪$,$p$)$^{21}$Na reaction is thought to be one of the key breakout reactions from the hot CNO cycles to the rp-process in type I x-ray bursts. In this work, the resonant properties of the compound nucleus $^{22}$Mg have been investigated by measuring the resonant elastic scattering of $^{21}$Na+$p$. An 89 MeV $^{21}$Na radioactive beam delivered from the CNS Radioactive Ion Beam Sep… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1403.4668v1-abstract-full').style.display = 'inline'; document.getElementById('1403.4668v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1403.4668v1-abstract-full" style="display: none;"> The $^{18}$Ne($伪$,$p$)$^{21}$Na reaction is thought to be one of the key breakout reactions from the hot CNO cycles to the rp-process in type I x-ray bursts. In this work, the resonant properties of the compound nucleus $^{22}$Mg have been investigated by measuring the resonant elastic scattering of $^{21}$Na+$p$. An 89 MeV $^{21}$Na radioactive beam delivered from the CNS Radioactive Ion Beam Separator bombarded an 8.8 mg/cm$^2$ thick polyethylene (CH$_{2}$)$_{n}$ target. The $^{21}$Na beam intensity was about 2$\times$10$^{5}$ pps, with a purity of about 70% on target. The recoiled protons were measured at the center-of-mass scattering angles of $胃_{c.m.}$$\approx$175.2${^\circ}$, 152.2${^\circ}$, and 150.5${^\circ}$ by three sets of $螖E$-$E$ telescopes, respectively. The excitation function was obtained with the thick-target method over energies $E_x$($^{22}$Mg)=5.5--9.2 MeV. In total, 23 states above the proton-threshold in $^{22}$Mg were observed, and their resonant parameters were determined via an $R$-matrix analysis of the excitation functions. We have made several new $J^蟺$ assignments and confirmed some tentative assignments made in previous work. The thermonuclear $^{18}$Ne($伪$,$p$)$^{21}$Na rate has been recalculated based on our recommended spin-parity assignments. The astrophysical impact of our new rate has been investigated through one-zone postprocessing x-ray burst calculations. We find that the $^{18}$Ne($伪$,$p$)$^{21}$Na rate significantly affects the peak nuclear energy generation rate, reaction fluxes, as well as the onset temperature of this breakout reaction in these astrophysical phenomena. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1403.4668v1-abstract-full').style.display = 'none'; document.getElementById('1403.4668v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 March, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2014. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1403.2127">arXiv:1403.2127</a> <span> [<a href="https://arxiv.org/pdf/1403.2127">pdf</a>, <a href="https://arxiv.org/ps/1403.2127">ps</a>, <a href="https://arxiv.org/format/1403.2127">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> Properties of resonant states in 18Ne relevant to key 14O(alpha,p)17F breakout reaction in type I x-ray bursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Hu%2C+J">J. Hu</a>, <a href="/search/nucl-ex?searchtype=author&query=He%2C+J+J">J. J. He</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Xu%2C+S+W">S. W. Xu</a>, <a href="/search/nucl-ex?searchtype=author&query=Yamaguchi%2C+H">H. Yamaguchi</a>, <a href="/search/nucl-ex?searchtype=author&query=Kahl%2C+D">D. Kahl</a>, <a href="/search/nucl-ex?searchtype=author&query=Ma%2C+P">P. Ma</a>, <a href="/search/nucl-ex?searchtype=author&query=Su%2C+J">J. Su</a>, <a href="/search/nucl-ex?searchtype=author&query=Wang%2C+H+W">H. W. Wang</a>, <a href="/search/nucl-ex?searchtype=author&query=Nakao%2C+T">T. Nakao</a>, <a href="/search/nucl-ex?searchtype=author&query=Wakabayashi%2C+Y">Y. Wakabayashi</a>, <a href="/search/nucl-ex?searchtype=author&query=Teranishi%2C+T">T. Teranishi</a>, <a href="/search/nucl-ex?searchtype=author&query=Hahn%2C+K+I">K. I. Hahn</a>, <a href="/search/nucl-ex?searchtype=author&query=Moon%2C+J+Y">J. Y. Moon</a>, <a href="/search/nucl-ex?searchtype=author&query=Sung%2C+H+S">H. S. Sung</a>, <a href="/search/nucl-ex?searchtype=author&query=Hashimoto%2C+T">T. Hashimoto</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+A+A">A. A. Chen</a>, <a href="/search/nucl-ex?searchtype=author&query=Irvine%2C+D">D. Irvine</a>, <a href="/search/nucl-ex?searchtype=author&query=Lee%2C+C+S">C. S. Lee</a>, <a href="/search/nucl-ex?searchtype=author&query=Kubono%2C+S">S. Kubono</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1403.2127v1-abstract-short" style="display: inline;"> The $^{14}$O($伪$,$p$)$^{17}$F reaction is one of the key reactions involved in the breakout from the hot-CNO cycle to the rp-process in type I x-ray bursts. The resonant properties in the compound nucleus $^{18}$Ne have been investigated through resonant elastic scattering of $^{17}$F+$p$. The radioactive $^{17}$F beam was separated by the CNS Radioactive Ion Beam separator (CRIB) and bombarded a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1403.2127v1-abstract-full').style.display = 'inline'; document.getElementById('1403.2127v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1403.2127v1-abstract-full" style="display: none;"> The $^{14}$O($伪$,$p$)$^{17}$F reaction is one of the key reactions involved in the breakout from the hot-CNO cycle to the rp-process in type I x-ray bursts. The resonant properties in the compound nucleus $^{18}$Ne have been investigated through resonant elastic scattering of $^{17}$F+$p$. The radioactive $^{17}$F beam was separated by the CNS Radioactive Ion Beam separator (CRIB) and bombarded a thick H$_2$ gas target at 3.6 MeV/nucleon. The recoiling light particles were measured by using three $螖$E-E silicon telescopes at laboratory angles of $胃$$_{lab}$$\approx$3$^\circ$, 10$^\circ$ and 18$^\circ$, respectively. Five resonances at $E_{x}$=6.15, 6.28, 6.35, 6.85, and 7.05 MeV were observed in the excitation functions. Based on an $R$-matrix analysis, $J^蟺$=1$^-$ was firmly assigned to the 6.15-MeV state. This state dominates the thermonuclear $^{14}$O($伪$,$p$)$^{17}$F rate below 1 GK. We have also confirmed the existence and spin-parities of three states between 6.1 and 6.4 MeV. As well, a possible new excited state in $^{18}$Ne was observed at $E_{x}$=6.85$\pm$0.11 MeV and tentatively assigned as $J$=0. This state could be the analog state of the 6.880 MeV (0$^{-}$) level in the mirror nucleus $^{18}$O, or a bandhead state (0$^+$) of the six-particle four-hole (6$p$-4$h$) band. A new thermonuclear rate of the $^{14}$O($伪$,$p$)$^{17}$F reaction has been determined, and its astrophysical impact has been examined within the framework of one-zone x-ray burst postprocessing calculations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1403.2127v1-abstract-full').style.display = 'none'; document.getElementById('1403.2127v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 March, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2014. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1312.0894">arXiv:1312.0894</a> <span> [<a href="https://arxiv.org/pdf/1312.0894">pdf</a>, <a href="https://arxiv.org/ps/1312.0894">ps</a>, <a href="https://arxiv.org/format/1312.0894">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.88.062802">10.1103/PhysRevC.88.062802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for new resonant states in 10C and 11C and their impact on the cosmological lithium problem </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Hammache%2C+F">F. Hammache</a>, <a href="/search/nucl-ex?searchtype=author&query=Coc%2C+A">A. Coc</a>, <a href="/search/nucl-ex?searchtype=author&query=de+S%C3%A9r%C3%A9ville%2C+N">N. de S茅r茅ville</a>, <a href="/search/nucl-ex?searchtype=author&query=Stefan%2C+I">I. Stefan</a>, <a href="/search/nucl-ex?searchtype=author&query=Roussel%2C+P">P. Roussel</a>, <a href="/search/nucl-ex?searchtype=author&query=Ancelin%2C+S">S. Ancelin</a>, <a href="/search/nucl-ex?searchtype=author&query=Assi%C3%A9%2C+M">M. Assi茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Audouin%2C+L">L. Audouin</a>, <a href="/search/nucl-ex?searchtype=author&query=Beaumel%2C+D">D. Beaumel</a>, <a href="/search/nucl-ex?searchtype=author&query=Franchoo%2C+S">S. Franchoo</a>, <a href="/search/nucl-ex?searchtype=author&query=Fernandez-Dominguez%2C+B">B. Fernandez-Dominguez</a>, <a href="/search/nucl-ex?searchtype=author&query=Fox%2C+S">S. Fox</a>, <a href="/search/nucl-ex?searchtype=author&query=Hamadache%2C+C">C. Hamadache</a>, <a href="/search/nucl-ex?searchtype=author&query=Kiener%2C+J">J. Kiener</a>, <a href="/search/nucl-ex?searchtype=author&query=Laird%2C+A">A. Laird</a>, <a href="/search/nucl-ex?searchtype=author&query=Crom%2C+B+L">B. Le Crom</a>, <a href="/search/nucl-ex?searchtype=author&query=Lefebvre-Schuhl%2C+A">A. Lefebvre-Schuhl</a>, <a href="/search/nucl-ex?searchtype=author&query=Lefebvre%2C+L">L. Lefebvre</a>, <a href="/search/nucl-ex?searchtype=author&query=Matea%2C+I">I. Matea</a>, <a href="/search/nucl-ex?searchtype=author&query=Matta%2C+A">A. Matta</a>, <a href="/search/nucl-ex?searchtype=author&query=Mavilla%2C+G">G. Mavilla</a>, <a href="/search/nucl-ex?searchtype=author&query=Mrazek%2C+J">J. Mrazek</a>, <a href="/search/nucl-ex?searchtype=author&query=Morfouace%2C+P">P. Morfouace</a>, <a href="/search/nucl-ex?searchtype=author&query=Santos%2C+F+d+O">F. de Oliveira Santos</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1312.0894v1-abstract-short" style="display: inline;"> The observed primordial 7Li abundance in metal-poor halo stars is found to be lower than its Big-Bang nucleosynthesis (BBN) calculated value by a factor of approximately three. Some recent works suggested the possibility that this discrepancy originates from missing resonant reactions which would destroy the 7Be, parent of 7Li. The most promising candidate resonances which were found include a pos… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.0894v1-abstract-full').style.display = 'inline'; document.getElementById('1312.0894v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1312.0894v1-abstract-full" style="display: none;"> The observed primordial 7Li abundance in metal-poor halo stars is found to be lower than its Big-Bang nucleosynthesis (BBN) calculated value by a factor of approximately three. Some recent works suggested the possibility that this discrepancy originates from missing resonant reactions which would destroy the 7Be, parent of 7Li. The most promising candidate resonances which were found include a possibly missed 1- or 2- narrow state around 15 MeV in the compound nucleus 10C formed by 7Be+3He and a state close to 7.8 MeV in the compound nucleus 11C formed by 7Be+4He. In this work, we studied the high excitation energy region of 10C and the low excitation energy region in 11C via the reactions 10B(3He,t)10C and 11B(3He,t)11C, respectively, at the incident energy of 35 MeV. Our results for 10C do not support 7Be+3He as a possible solution for the 7Li problem. Concerning 11C results, the data show no new resonances in the excitation energy region of interest and this excludes 7Be+4He reaction channel as an explanation for the 7Li deficit. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.0894v1-abstract-full').style.display = 'none'; document.getElementById('1312.0894v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 December, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Phys. Rev. C (Rapid Communication)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1309.3543">arXiv:1309.3543</a> <span> [<a href="https://arxiv.org/pdf/1309.3543">pdf</a>, <a href="https://arxiv.org/format/1309.3543">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.88.045801">10.1103/PhysRevC.88.045801 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraining nova observables: direct measurements of resonance strengths in 33S(p,纬)34Cl </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Fallis%2C+J">J. Fallis</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Bertone%2C+P+F">P. F. Bertone</a>, <a href="/search/nucl-ex?searchtype=author&query=Bishop%2C+S">S. Bishop</a>, <a href="/search/nucl-ex?searchtype=author&query=Buchmann%2C+L">L. Buchmann</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+A+A">A. A. Chen</a>, <a href="/search/nucl-ex?searchtype=author&query=Christian%2C+G">G. Christian</a>, <a href="/search/nucl-ex?searchtype=author&query=Clark%2C+J+A">J. A. Clark</a>, <a href="/search/nucl-ex?searchtype=author&query=D%27Auria%2C+J+M">J. M. D'Auria</a>, <a href="/search/nucl-ex?searchtype=author&query=Davids%2C+B">B. Davids</a>, <a href="/search/nucl-ex?searchtype=author&query=Deibel%2C+C+M">C. M. Deibel</a>, <a href="/search/nucl-ex?searchtype=author&query=Fulton%2C+B+R">B. R. Fulton</a>, <a href="/search/nucl-ex?searchtype=author&query=Greife%2C+U">U. Greife</a>, <a href="/search/nucl-ex?searchtype=author&query=Guo%2C+B">B. Guo</a>, <a href="/search/nucl-ex?searchtype=author&query=Hager%2C+U">U. Hager</a>, <a href="/search/nucl-ex?searchtype=author&query=Herlitzius%2C+C">C. Herlitzius</a>, <a href="/search/nucl-ex?searchtype=author&query=Hutcheon%2C+D+A">D. A. Hutcheon</a>, <a href="/search/nucl-ex?searchtype=author&query=Jos%C3%A9%2C+J">J. Jos茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Laird%2C+A+M">A. M. Laird</a>, <a href="/search/nucl-ex?searchtype=author&query=Li%2C+E+T">E. T. Li</a>, <a href="/search/nucl-ex?searchtype=author&query=Li%2C+Z+H">Z. H. Li</a>, <a href="/search/nucl-ex?searchtype=author&query=Lian%2C+G">G. Lian</a>, <a href="/search/nucl-ex?searchtype=author&query=Liu%2C+W+P">W. P. Liu</a>, <a href="/search/nucl-ex?searchtype=author&query=Martin%2C+L">L. Martin</a>, <a href="/search/nucl-ex?searchtype=author&query=Nelson%2C+K">K. Nelson</a> , et al. (10 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1309.3543v1-abstract-short" style="display: inline;"> The 33S(p,纬)34Cl reaction is important for constraining predictions of certain isotopic abundances in oxygen-neon novae. Models currently predict as much as 150 times the solar abundance of 33S in oxygen-neon nova ejecta. This overproduction factor may, however, vary by orders of magnitude due to uncertainties in the 33S(p,纬)34Cl reaction rate at nova peak temperatures. Depending on this rate, 33S… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1309.3543v1-abstract-full').style.display = 'inline'; document.getElementById('1309.3543v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1309.3543v1-abstract-full" style="display: none;"> The 33S(p,纬)34Cl reaction is important for constraining predictions of certain isotopic abundances in oxygen-neon novae. Models currently predict as much as 150 times the solar abundance of 33S in oxygen-neon nova ejecta. This overproduction factor may, however, vary by orders of magnitude due to uncertainties in the 33S(p,纬)34Cl reaction rate at nova peak temperatures. Depending on this rate, 33S could potentially be used as a diagnostic tool for classifying certain types of presolar grains. Better knowledge of the 33S(p,纬)34Cl rate would also aid in interpreting nova observations over the S-Ca mass region and contribute to the firm establishment of the maximum endpoint of nova nucleosynthesis. Additionally, the total S elemental abundance which is affected by this reaction has been proposed as a thermometer to study the peak temperatures of novae. Previously, the 33S(p,纬)34Cl reaction rate had only been studied directly down to resonance energies of 432 keV. However, for nova peak temperatures of 0.2-0.4 GK there are 7 known states in 34Cl both below the 432 keV resonance and within the Gamow window that could play a dominant role. Direct measurements of the resonance strengths of these states were performed using the DRAGON recoil separator at TRIUMF. Additionally two new states within this energy region are reported. Several hydrodynamic simulations have been performed, using all available experimental information for the 33S(p,纬)34Cl rate, to explore the impact of the remaining uncertainty in this rate on nucleosynthesis in nova explosions. These calculations give a range of ~ 20-150 for the expected 33S overproduction factor, and a range of ~ 100-450 for the 32S/33S ratio expected in ONe novae. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1309.3543v1-abstract-full').style.display = 'none'; document.getElementById('1309.3543v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 September, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 8 figures, Accepted for publication in Physical Review C</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1306.6007">arXiv:1306.6007</a> <span> [<a href="https://arxiv.org/pdf/1306.6007">pdf</a>, <a href="https://arxiv.org/ps/1306.6007">ps</a>, <a href="https://arxiv.org/format/1306.6007">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/201321518">10.1051/0004-6361/201321518 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Effects of Variations in Nuclear Interactions on Nucleosynthesis in Thermonuclear Supernovae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">Anuj Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Jose%2C+J">Jordi Jose</a>, <a href="/search/nucl-ex?searchtype=author&query=Seitenzahl%2C+I+R">Ivo R. Seitenzahl</a>, <a href="/search/nucl-ex?searchtype=author&query=Roepke%2C+F+K">Friedrich K. Roepke</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1306.6007v1-abstract-short" style="display: inline;"> The impact of nuclear physics uncertainties on nucleosynthesis in thermonuclear supernovae has not been fully explored using comprehensive and systematic studies with multiple models. To better constrain predictions of yields from these phenomena, we have performed a sensitivity study by post-processing thermodynamic histories from two different hydrodynamic, Chandrasekhar-mass explosion models. W… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1306.6007v1-abstract-full').style.display = 'inline'; document.getElementById('1306.6007v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1306.6007v1-abstract-full" style="display: none;"> The impact of nuclear physics uncertainties on nucleosynthesis in thermonuclear supernovae has not been fully explored using comprehensive and systematic studies with multiple models. To better constrain predictions of yields from these phenomena, we have performed a sensitivity study by post-processing thermodynamic histories from two different hydrodynamic, Chandrasekhar-mass explosion models. We have individually varied all input reaction and, for the first time, weak interaction rates by a factor of ten and compared the yields in each case to yields using standard rates. Of the 2305 nuclear reactions in our network, we find that the rates of only 53 reactions affect the yield of any species with an abundance of at least 10^-8 M_sun by at least a factor of two, in either model. The rates of the 12C(a,g), 12C+12C, 20Ne(a,p), 20Ne(a,g) and 30Si(p,g) reactions are among those that modify the most yields when varied by a factor of ten. From the individual variation of 658 weak interaction rates in our network by a factor of ten, only the stellar 28Si(b+)28Al, 32S(b+)32P and 36Ar(b+)36Cl rates significantly affect the yields of species in a model. Additional tests reveal that reaction rate changes over temperatures T > 1.5 GK have the greatest impact, and that ratios of radionuclides that may be used as explosion diagnostics change by a factor of less than two from the variation of individual rates by a factor of 10. Nucleosynthesis in the two adopted models is relatively robust to variations in individual nuclear reaction and weak interaction rates. Laboratory measurements of a limited number of reactions would help to further constrain predictions. As well, we confirm the need for a consistent treatment for relevant stellar weak interaction rates since simultaneous variation of these rates (as opposed to individual variation) has a significant effect on yields in our models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1306.6007v1-abstract-full').style.display = 'none'; document.getElementById('1306.6007v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 June, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted by A&A, 14 pages, 5 figures, 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1301.4283">arXiv:1301.4283</a> <span> [<a href="https://arxiv.org/pdf/1301.4283">pdf</a>, <a href="https://arxiv.org/ps/1301.4283">ps</a>, <a href="https://arxiv.org/format/1301.4283">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.88.012801">10.1103/PhysRevC.88.012801 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The 18Ne(a,p)21Na breakout reaction in x-ray bursts: experimental determination of spin-parities for alpha resonances in 22Mg via resonant elastic scattering of 21Na+p </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=He%2C+J+J">J. J. He</a>, <a href="/search/nucl-ex?searchtype=author&query=Zhang%2C+L+Y">L. Y. Zhang</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Xu%2C+S+W">S. W. Xu</a>, <a href="/search/nucl-ex?searchtype=author&query=Yamaguchi%2C+H">H. Yamaguchi</a>, <a href="/search/nucl-ex?searchtype=author&query=Kahl%2C+D">D. Kahl</a>, <a href="/search/nucl-ex?searchtype=author&query=Kubono%2C+S">S. Kubono</a>, <a href="/search/nucl-ex?searchtype=author&query=Hu%2C+J">J. Hu</a>, <a href="/search/nucl-ex?searchtype=author&query=Ma%2C+P">P. Ma</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+S+Z">S. Z. Chen</a>, <a href="/search/nucl-ex?searchtype=author&query=Wakabayashi%2C+Y">Y. Wakabayashi</a>, <a href="/search/nucl-ex?searchtype=author&query=Sun%2C+B+H">B. H. Sun</a>, <a href="/search/nucl-ex?searchtype=author&query=Wang%2C+H+W">H. W. Wang</a>, <a href="/search/nucl-ex?searchtype=author&query=Tian%2C+W+D">W. D. Tian</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+R+F">R. F. Chen</a>, <a href="/search/nucl-ex?searchtype=author&query=Guo%2C+B">B. Guo</a>, <a href="/search/nucl-ex?searchtype=author&query=Hashimoto%2C+T">T. Hashimoto</a>, <a href="/search/nucl-ex?searchtype=author&query=Togano%2C+Y">Y. Togano</a>, <a href="/search/nucl-ex?searchtype=author&query=Hayakawa%2C+S">S. Hayakawa</a>, <a href="/search/nucl-ex?searchtype=author&query=Teranishi%2C+T">T. Teranishi</a>, <a href="/search/nucl-ex?searchtype=author&query=Iwasa%2C+N">N. Iwasa</a>, <a href="/search/nucl-ex?searchtype=author&query=Yamada%2C+T">T. Yamada</a>, <a href="/search/nucl-ex?searchtype=author&query=Komatsubara%2C+T">T. Komatsubara</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1301.4283v2-abstract-short" style="display: inline;"> The $^{18}$Ne($伪$,$p$)$^{21}$Na reaction provides a pathway for breakout from the hot CNO cycles to the $rp$-process in type I x-ray bursts. To better determine this astrophysical reaction rate, the resonance parameters of the compound nucleus $^{22}$Mg have been investigated by measuring the resonant elastic scattering of $^{21}$Na+$p$. An 89 MeV $^{21}$Na radioactive ion beam was produced at the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1301.4283v2-abstract-full').style.display = 'inline'; document.getElementById('1301.4283v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1301.4283v2-abstract-full" style="display: none;"> The $^{18}$Ne($伪$,$p$)$^{21}$Na reaction provides a pathway for breakout from the hot CNO cycles to the $rp$-process in type I x-ray bursts. To better determine this astrophysical reaction rate, the resonance parameters of the compound nucleus $^{22}$Mg have been investigated by measuring the resonant elastic scattering of $^{21}$Na+$p$. An 89 MeV $^{21}$Na radioactive ion beam was produced at the CNS Radioactive Ion Beam Separator and bombarded an 8.8 mg/cm$^2$ thick polyethylene target. The recoiled protons were measured at scattering angles of $胃_{c.m.}$$\approx 175 {^\circ}$ and 152${^\circ}$ by three $螖E$-$E$ silicon telescopes. The excitation function was obtained with a thick-target method over energies $E_x$($^{22}$Mg)=5.5--9.2 MeV. The resonance parameters have been determined through an $R$-matrix analysis. For the first time, the $J^蟺$ values for ten states above the alpha threshold in $^{22}$Mg have been experimentally determined in a single consistent measurement. We have made three new $J^蟺$ assignments and confirmed seven of the ten tentative assignments in the previous work. The $^{18}$Ne($伪$,$p$)$^{21}$Na reaction rate has been recalculated, and the astrophysical impact of our new rate has been investigated through one-zone postprocessing x-ray burst calculations. We find that the $^{18}$Ne($伪$,$p$)$^{21}$Na rate significantly affects the peak nuclear energy generation rate and the onset temperature of this breakout reaction in these phenomena. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1301.4283v2-abstract-full').style.display = 'none'; document.getElementById('1301.4283v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 July, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 January, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 4 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1212.2367">arXiv:1212.2367</a> <span> [<a href="https://arxiv.org/pdf/1212.2367">pdf</a>, <a href="https://arxiv.org/format/1212.2367">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.110.032502">10.1103/PhysRevLett.110.032502 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Is 纬-ray emission from novae affected by interference effects in the 18F(p,伪)15O reaction? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Laird%2C+A+M">A. M. Laird</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Murphy%2C+A+S+J">A. St. J. Murphy</a>, <a href="/search/nucl-ex?searchtype=author&query=Wimmer%2C+K">K. Wimmer</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+A+A">A. A. Chen</a>, <a href="/search/nucl-ex?searchtype=author&query=Deibel%2C+C+M">C. M. Deibel</a>, <a href="/search/nucl-ex?searchtype=author&query=Faestermann%2C+T">T. Faestermann</a>, <a href="/search/nucl-ex?searchtype=author&query=Fox%2C+S+P">S. P. Fox</a>, <a href="/search/nucl-ex?searchtype=author&query=Fulton%2C+B+R">B. R. Fulton</a>, <a href="/search/nucl-ex?searchtype=author&query=Hertenberger%2C+R">R. Hertenberger</a>, <a href="/search/nucl-ex?searchtype=author&query=Irvine%2C+D">D. Irvine</a>, <a href="/search/nucl-ex?searchtype=author&query=Jos%C3%A9%2C+J">J. Jos茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Longland%2C+R">R. Longland</a>, <a href="/search/nucl-ex?searchtype=author&query=Mountford%2C+D">D. Mountford</a>, <a href="/search/nucl-ex?searchtype=author&query=Sambrook%2C+B">B. Sambrook</a>, <a href="/search/nucl-ex?searchtype=author&query=Seiler%2C+D">D. Seiler</a>, <a href="/search/nucl-ex?searchtype=author&query=Wirth%2C+H+-">H. -F. Wirth</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1212.2367v1-abstract-short" style="display: inline;"> The 18F(p,伪)15O reaction rate is crucial for constraining model predictions of the 纬-ray observable radioisotope 18F produced in novae. The determination of this rate is challenging due to particular features of the level scheme of the compound nucleus, 19Ne, which result in interference effects potentially playing a significant role. The dominant uncertainty in this rate arises from interference… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1212.2367v1-abstract-full').style.display = 'inline'; document.getElementById('1212.2367v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1212.2367v1-abstract-full" style="display: none;"> The 18F(p,伪)15O reaction rate is crucial for constraining model predictions of the 纬-ray observable radioisotope 18F produced in novae. The determination of this rate is challenging due to particular features of the level scheme of the compound nucleus, 19Ne, which result in interference effects potentially playing a significant role. The dominant uncertainty in this rate arises from interference between J蟺=3/2+ states near the proton threshold (Sp = 6.411 MeV) and a broad J蟺=3/2+ state at 665 keV above threshold. This unknown interference term results in up to a factor of 40 uncertainty in the astrophysical S-factor at nova temperatures. Here we report a new measurement of states in this energy region using the 19F(3He,t)19Ne reaction. In stark contrast with previous assumptions we find at least 3 resonances between the proton threshold and Ecm=50 keV, all with different angular distributions. None of these are consistent with J蟺= 3/2+ angular distributions. We find that the main uncertainty now arises from the unknown proton-width of the 48 keV resonance, not from possible interference effects. Hydrodynamic nova model calculations performed indicate that this unknown width affects 18F production by at least a factor of two in the model considered. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1212.2367v1-abstract-full').style.display = 'none'; document.getElementById('1212.2367v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 December, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 4 figures. Accepted for publication in Phys. Rev. Lett</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1211.5900">arXiv:1211.5900</a> <span> [<a href="https://arxiv.org/pdf/1211.5900">pdf</a>, <a href="https://arxiv.org/format/1211.5900">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.ppnp.2012.11.002">10.1016/j.ppnp.2012.11.002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Nucleosynthesis in Type I X-ray Bursts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Jos%C3%A9%2C+J">J. Jos茅</a>, <a href="/search/nucl-ex?searchtype=author&query=Sala%2C+G">G. Sala</a>, <a href="/search/nucl-ex?searchtype=author&query=Iliadis%2C+C">C. Iliadis</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1211.5900v1-abstract-short" style="display: inline;"> Type I X-ray bursts are thermonuclear explosions that occur in the envelopes of accreting neutron stars. Detailed observations of these phenomena have prompted numerous studies in theoretical astrophysics and experimental nuclear physics since their discovery over 35 years ago. In this review, we begin by discussing key observational features of these phenomena that may be sensitive to the particu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.5900v1-abstract-full').style.display = 'inline'; document.getElementById('1211.5900v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1211.5900v1-abstract-full" style="display: none;"> Type I X-ray bursts are thermonuclear explosions that occur in the envelopes of accreting neutron stars. Detailed observations of these phenomena have prompted numerous studies in theoretical astrophysics and experimental nuclear physics since their discovery over 35 years ago. In this review, we begin by discussing key observational features of these phenomena that may be sensitive to the particular patterns of nucleosynthesis from the associated thermonuclear burning. We then summarize efforts to model type I X-ray bursts, with emphasis on determining the nuclear physics processes involved throughout these bursts. We discuss and evaluate limitations in the models, particularly with regard to key uncertainties in the nuclear physics input. Finally, we examine recent, relevant experimental measurements and outline future prospects to improve our understanding of these unique environments from observational, theoretical and experimental perspectives. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1211.5900v1-abstract-full').style.display = 'none'; document.getElementById('1211.5900v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 November, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by Prog. Part. Nucl. Phys., 45 pages, 14 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1112.3181">arXiv:1112.3181</a> <span> [<a href="https://arxiv.org/pdf/1112.3181">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.84.065808">10.1103/PhysRevC.84.065808 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Production of 26Al in stellar hydrogen-burning environments: spectroscopic properties of states in 27Si </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Wimmer%2C+K">K. Wimmer</a>, <a href="/search/nucl-ex?searchtype=author&query=Faestermann%2C+T">T. Faestermann</a>, <a href="/search/nucl-ex?searchtype=author&query=Hertenberger%2C+R">R. Hertenberger</a>, <a href="/search/nucl-ex?searchtype=author&query=Wirth%2C+H+-">H. -F. Wirth</a>, <a href="/search/nucl-ex?searchtype=author&query=Chen%2C+A+A">A. A. Chen</a>, <a href="/search/nucl-ex?searchtype=author&query=Clark%2C+J+A">J. A. Clark</a>, <a href="/search/nucl-ex?searchtype=author&query=Deibel%2C+C+M">C. M. Deibel</a>, <a href="/search/nucl-ex?searchtype=author&query=Herlitzius%2C+C">C. Herlitzius</a>, <a href="/search/nucl-ex?searchtype=author&query=Krucken%2C+R">R. Krucken</a>, <a href="/search/nucl-ex?searchtype=author&query=Seiler%2C+D">D. Seiler</a>, <a href="/search/nucl-ex?searchtype=author&query=Setoodehnia%2C+K">K. Setoodehnia</a>, <a href="/search/nucl-ex?searchtype=author&query=Straub%2C+K">K. Straub</a>, <a href="/search/nucl-ex?searchtype=author&query=Wrede%2C+C">C. Wrede</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1112.3181v1-abstract-short" style="display: inline;"> Model predictions of the amount of the radioisotope 26Al produced in hydrogen-burning environments require reliable estimates of the thermonuclear rates for the 26gAl(p,纬)27Si and 26mAl(p,纬)27Si reactions. These rates depend upon the spectroscopic properties of states in 27Si within about 1 MeV of the 26gAl+p threshold (Sp = 7463 keV). We have studied the 28Si(3He,伪)27Si reaction at 25 MeV using a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1112.3181v1-abstract-full').style.display = 'inline'; document.getElementById('1112.3181v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1112.3181v1-abstract-full" style="display: none;"> Model predictions of the amount of the radioisotope 26Al produced in hydrogen-burning environments require reliable estimates of the thermonuclear rates for the 26gAl(p,纬)27Si and 26mAl(p,纬)27Si reactions. These rates depend upon the spectroscopic properties of states in 27Si within about 1 MeV of the 26gAl+p threshold (Sp = 7463 keV). We have studied the 28Si(3He,伪)27Si reaction at 25 MeV using a high-resolution quadrupole-dipole-dipole-dipole magnetic spectrograph. For the first time with a transfer reaction, we have constrained J蟺 values for states in 27Si over Ex = 7.0 - 8.1 MeV through angular distribution measurements. Aside from a few important cases, we generally confirm the energies and spin-parity assignments reported in a recent 纬-ray spectroscopy study. The magnitudes of neutron spectroscopic factors determined from shell-model calculations are in reasonable agreement with our experimental values extracted using this reaction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1112.3181v1-abstract-full').style.display = 'none'; document.getElementById('1112.3181v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 December, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for publication in Phys. Rev. C</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1101.0643">arXiv:1101.0643</a> <span> [<a href="https://arxiv.org/pdf/1101.0643">pdf</a>, <a href="https://arxiv.org/ps/1101.0643">ps</a>, <a href="https://arxiv.org/format/1101.0643">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.83.048801">10.1103/PhysRevC.83.048801 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Branches of 33S(p,纬)34Cl at Oxygen-Neon Nova Temperatures </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Freeman%2C+B+M">B. M. Freeman</a>, <a href="/search/nucl-ex?searchtype=author&query=Wrede%2C+C">C. Wrede</a>, <a href="/search/nucl-ex?searchtype=author&query=Delbridge%2C+B+G">B. G. Delbridge</a>, <a href="/search/nucl-ex?searchtype=author&query=Garcia%2C+A">A. Garcia</a>, <a href="/search/nucl-ex?searchtype=author&query=Knecht%2C+A">A. Knecht</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Sallaska%2C+A+L">A. L. Sallaska</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1101.0643v2-abstract-short" style="display: inline;"> Recent simulations of classical novae on oxygen-neon white-dwarf stars indicate that the isotopic ratio 32S/33S has the potential to be a remarkable indicator of presolar grains of nova origin. The 33S(p,纬)34Cl reaction influences this ratio directly by destroying 33S in novae. Additionally, 尾-delayed 纬-rays from the metastable state of 34Cl (t_{1/2} = 32 min) have been suggested to be potential n… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1101.0643v2-abstract-full').style.display = 'inline'; document.getElementById('1101.0643v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1101.0643v2-abstract-full" style="display: none;"> Recent simulations of classical novae on oxygen-neon white-dwarf stars indicate that the isotopic ratio 32S/33S has the potential to be a remarkable indicator of presolar grains of nova origin. The 33S(p,纬)34Cl reaction influences this ratio directly by destroying 33S in novae. Additionally, 尾-delayed 纬-rays from the metastable state of 34Cl (t_{1/2} = 32 min) have been suggested to be potential nova observables. We have measured the branches for known 33S(p,纬)34Cl resonances that are activated at temperatures relevant to oxygen-neon novae. We provide the first reliable uncertainties on these branches and the first upper limits for several previously unmeasured branches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1101.0643v2-abstract-full').style.display = 'none'; document.getElementById('1101.0643v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 May, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 January, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.C83:048801,2011 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1005.4767">arXiv:1005.4767</a> <span> [<a href="https://arxiv.org/pdf/1005.4767">pdf</a>, <a href="https://arxiv.org/ps/1005.4767">ps</a>, <a href="https://arxiv.org/format/1005.4767">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0067-0049/189/1/204">10.1088/0067-0049/189/1/204 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Hydrodynamic Models of Type I X-Ray Bursts: Metallicity Effects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Jose%2C+J">Jordi Jose</a>, <a href="/search/nucl-ex?searchtype=author&query=Moreno%2C+F">Fermin Moreno</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">Anuj Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Iliadis%2C+C">Christian Iliadis</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1005.4767v1-abstract-short" style="display: inline;"> Type I X-ray bursts are thermonuclear stellar explosions driven by charged-particle reactions. In the regime for combined H/He-ignition, the main nuclear flow is dominated by the rp-process (rapid proton-captures and beta+ decays), the 3 alpha-reaction, and the alpha-p-process (a suite of (alpha,p) and (p,gamma) reactions). The main flow is expected to proceed away from the valley of stability, ev… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1005.4767v1-abstract-full').style.display = 'inline'; document.getElementById('1005.4767v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1005.4767v1-abstract-full" style="display: none;"> Type I X-ray bursts are thermonuclear stellar explosions driven by charged-particle reactions. In the regime for combined H/He-ignition, the main nuclear flow is dominated by the rp-process (rapid proton-captures and beta+ decays), the 3 alpha-reaction, and the alpha-p-process (a suite of (alpha,p) and (p,gamma) reactions). The main flow is expected to proceed away from the valley of stability, eventually reaching the proton drip-line beyond A = 38. Detailed analysis of the relevant reactions along the main path has only been scarcely addressed, mainly in the context of parameterized one-zone models. In this paper, we present a detailed study of the nucleosynthesis and nuclear processes powering type I X-ray bursts. The reported 11 bursts have been computed by means of a spherically symmetric (1D), Lagrangian, hydrodynamic code, linked to a nuclear reaction network that contains 325 isotopes (from 1H to 107Te), and 1392 nuclear processes. These evolutionary sequences, followed from the onset of accretion up to the explosion and expansion stages, have been performed for 2 different metallicities to explore the dependence between the extension of the main nuclear flow and the initial metal content. We carefully analyze the dominant reactions and the products of nucleosynthesis, together with the the physical parameters that determine the light curve (including recurrence times, ratios between persistent and burst luminosities, or the extent of the envelope expansion). Results are in qualitative agreement with the observed properties of some well-studied bursting sources. Leakage from the predicted SbSnTe-cycle cannot be discarded in some of our models. Production of 12C (and implications for the mechanism that powers superbursts), light p-nuclei, and the amount of H left over after the bursting episodes will also be discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1005.4767v1-abstract-full').style.display = 'none'; document.getElementById('1005.4767v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 May, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">78 pages (pdf), including 34 figures. Accepted for publication in The Astrophysical Journal Suppl. Series</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0906.3610">arXiv:0906.3610</a> <span> [<a href="https://arxiv.org/pdf/0906.3610">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.80.015802">10.1103/PhysRevC.80.015802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> New 34Cl proton-threshold states and the thermonuclear 33S(p,gamma)34Cl rate in ONe novae </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Faestermann%2C+T">T. Faestermann</a>, <a href="/search/nucl-ex?searchtype=author&query=Hertenberger%2C+R">R. Hertenberger</a>, <a href="/search/nucl-ex?searchtype=author&query=Kruecken%2C+R">R. Kruecken</a>, <a href="/search/nucl-ex?searchtype=author&query=Schafstadler%2C+D">D. Schafstadler</a>, <a href="/search/nucl-ex?searchtype=author&query=Wirth%2C+H+-">H. -F. Wirth</a>, <a href="/search/nucl-ex?searchtype=author&query=Behrens%2C+T">T. Behrens</a>, <a href="/search/nucl-ex?searchtype=author&query=Bildstein%2C+V">V. Bildstein</a>, <a href="/search/nucl-ex?searchtype=author&query=Bishop%2C+S">S. Bishop</a>, <a href="/search/nucl-ex?searchtype=author&query=Eppinger%2C+K">K. Eppinger</a>, <a href="/search/nucl-ex?searchtype=author&query=Herlitzius%2C+C">C. Herlitzius</a>, <a href="/search/nucl-ex?searchtype=author&query=Hinke%2C+C">C. Hinke</a>, <a href="/search/nucl-ex?searchtype=author&query=Schlarb%2C+M">M. Schlarb</a>, <a href="/search/nucl-ex?searchtype=author&query=Seiler%2C+D">D. Seiler</a>, <a href="/search/nucl-ex?searchtype=author&query=Wimmer%2C+K">K. Wimmer</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0906.3610v1-abstract-short" style="display: inline;"> Analysis of presolar grains in primitive meteorites has shown isotopic ratios largely characteristic of the conditions thought to prevail in various astrophysical environments. A possible indicator for a grain of ONe nova origin is a large 33S abundance: nucleosynthesis calculations predict as much as 150 times the solar abundance of 33S in the ejecta of nova explosions on massive ONe white dwar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0906.3610v1-abstract-full').style.display = 'inline'; document.getElementById('0906.3610v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0906.3610v1-abstract-full" style="display: none;"> Analysis of presolar grains in primitive meteorites has shown isotopic ratios largely characteristic of the conditions thought to prevail in various astrophysical environments. A possible indicator for a grain of ONe nova origin is a large 33S abundance: nucleosynthesis calculations predict as much as 150 times the solar abundance of 33S in the ejecta of nova explosions on massive ONe white dwarfs. This overproduction factor may, however, vary by factors of at least 0.01 - 3 because of uncertainties of several orders of magnitude in the 33S(p,gamma)34Cl reaction rate at nova peak temperatures (Tpeak ~ 0.1 - 0.4 GK). These uncertainties arise due to the lack of nuclear physics information for states within ~ 600 keV of the 33S+p threshold in 34Cl (Sp(34Cl) = 5143 keV). To better constrain this rate we have measured, for the first time, the 34S(3He,t)34Cl reaction over the region Ex(34Cl) = 4.9 - 6 MeV. We confirm previous states and find 15 new states in this energy region. New 33S(p,gamma)34Cl resonances at ER = 281(2), 301(2) and 342(2) keV may dominate this rate at relevant nova temperatures. Our results could affect predictions of sulphur isotopic ratios in nova ejecta (e.g., 32S/33S) that may be used as diagnostic tools for the nova paternity of grains. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0906.3610v1-abstract-full').style.display = 'none'; document.getElementById('0906.3610v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 June, 2009; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2009. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">accepted for Phys. Rev. C, 2 tables, 2 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.C80:015802,2009 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0710.0719">arXiv:0710.0719</a> <span> [<a href="https://arxiv.org/pdf/0710.0719">pdf</a>, <a href="https://arxiv.org/ps/0710.0719">ps</a>, <a href="https://arxiv.org/format/0710.0719">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.100.112501">10.1103/PhysRevLett.100.112501 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Nuclear Structure Relevant to Neutrinoless Double Beta Decay: 76Ge and 76Se </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Schiffer%2C+J+P">J. P. Schiffer</a>, <a href="/search/nucl-ex?searchtype=author&query=Freeman%2C+S+J">S. J. Freeman</a>, <a href="/search/nucl-ex?searchtype=author&query=Clark%2C+J+A">J. A. Clark</a>, <a href="/search/nucl-ex?searchtype=author&query=Deibel%2C+C">C. Deibel</a>, <a href="/search/nucl-ex?searchtype=author&query=Fitzpatrick%2C+C+R">C. R. Fitzpatrick</a>, <a href="/search/nucl-ex?searchtype=author&query=Gros%2C+S">S. Gros</a>, <a href="/search/nucl-ex?searchtype=author&query=Heinz%2C+A">A. Heinz</a>, <a href="/search/nucl-ex?searchtype=author&query=Hirata%2C+D">D. Hirata</a>, <a href="/search/nucl-ex?searchtype=author&query=Jiang%2C+C+L">C. L. Jiang</a>, <a href="/search/nucl-ex?searchtype=author&query=Kay%2C+B+P">B. P. Kay</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Parker%2C+P+D">P. D. Parker</a>, <a href="/search/nucl-ex?searchtype=author&query=Rehm%2C+K+E">K. E. Rehm</a>, <a href="/search/nucl-ex?searchtype=author&query=Villari%2C+A+C+C">A. C. C. Villari</a>, <a href="/search/nucl-ex?searchtype=author&query=Werner%2C+V">V. Werner</a>, <a href="/search/nucl-ex?searchtype=author&query=Wrede%2C+C">C. Wrede</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0710.0719v1-abstract-short" style="display: inline;"> The possibility of observing neutrinoless double beta decay offers the opportunity of determining the neutrino mass IF the nuclear matrix element were known. Theoretical calculations are uncertain and measurements of the occupations of valence orbits by nucleons active in the decay can be important. The occupation of valence neutron orbits in the ground states of 76Ge and 76Se were determined by… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0710.0719v1-abstract-full').style.display = 'inline'; document.getElementById('0710.0719v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0710.0719v1-abstract-full" style="display: none;"> The possibility of observing neutrinoless double beta decay offers the opportunity of determining the neutrino mass IF the nuclear matrix element were known. Theoretical calculations are uncertain and measurements of the occupations of valence orbits by nucleons active in the decay can be important. The occupation of valence neutron orbits in the ground states of 76Ge and 76Se were determined by precisely measuring cross sections for both neutron-adding and removing transfer reactions. Our results indicate that the Fermi surface is much more diffuse than in theoretical (QRPA) calculations. We find that the populations of at least three orbits change significantly between these two ground states while in the calculations the changes are confined primarily to one orbit. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0710.0719v1-abstract-full').style.display = 'none'; document.getElementById('0710.0719v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 October, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 3 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.Lett.100:112501,2008 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0709.1743">arXiv:0709.1743</a> <span> [<a href="https://arxiv.org/pdf/0709.1743">pdf</a>, <a href="https://arxiv.org/ps/0709.1743">ps</a>, <a href="https://arxiv.org/format/0709.1743">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.76.025802">10.1103/PhysRevC.76.025802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Experimental evidence of a natural parity state in $^{26}$Mg and its impact to the production of neutrons for the s process </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Ugalde%2C+C">C. Ugalde</a>, <a href="/search/nucl-ex?searchtype=author&query=Champagne%2C+A+E">A. E. Champagne</a>, <a href="/search/nucl-ex?searchtype=author&query=Daigle%2C+S">S. Daigle</a>, <a href="/search/nucl-ex?searchtype=author&query=Iliadis%2C+C">C. Iliadis</a>, <a href="/search/nucl-ex?searchtype=author&query=Longland%2C+R">R. Longland</a>, <a href="/search/nucl-ex?searchtype=author&query=Newton%2C+J+R">J. R. Newton</a>, <a href="/search/nucl-ex?searchtype=author&query=Osenbaugh-Stewart%2C+E">E. Osenbaugh-Stewart</a>, <a href="/search/nucl-ex?searchtype=author&query=Clark%2C+J+A">J. A. Clark</a>, <a href="/search/nucl-ex?searchtype=author&query=Deibel%2C+C">C. Deibel</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Parker%2C+P+D">P. D. Parker</a>, <a href="/search/nucl-ex?searchtype=author&query=Wrede%2C+C">C. Wrede</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0709.1743v1-abstract-short" style="display: inline;"> We have studied natural parity states in $^{26}$Mg via the $^{22}$Ne($^{6}$Li,d)$^{26}$Mg reaction. Our method significantly improves the energy resolution of previous experiments and, as a result, we report the observation of a natural parity state in $^{26}$Mg. Possible spin-parity assignments are suggested on the basis of published $纬$-ray decay experiments. The stellar rate of the $^{22}$Ne(… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0709.1743v1-abstract-full').style.display = 'inline'; document.getElementById('0709.1743v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0709.1743v1-abstract-full" style="display: none;"> We have studied natural parity states in $^{26}$Mg via the $^{22}$Ne($^{6}$Li,d)$^{26}$Mg reaction. Our method significantly improves the energy resolution of previous experiments and, as a result, we report the observation of a natural parity state in $^{26}$Mg. Possible spin-parity assignments are suggested on the basis of published $纬$-ray decay experiments. The stellar rate of the $^{22}$Ne($伪$,$纬$)$^{26}$Mg reaction is reduced and may give rise to an increase in the production of s-process neutrons via the $^{22}$Ne($伪$,n)$^{25}$Mg reaction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0709.1743v1-abstract-full').style.display = 'none'; document.getElementById('0709.1743v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 September, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in PRC</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.C76:025802,2007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0709.0468">arXiv:0709.0468</a> <span> [<a href="https://arxiv.org/pdf/0709.0468">pdf</a>, <a href="https://arxiv.org/ps/0709.0468">ps</a>, <a href="https://arxiv.org/format/0709.0468">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.physletb.2007.11.033">10.1016/j.physletb.2007.11.033 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> High-j single-particle neutron states outside the N=82 core </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Kay%2C+B+P">B. P. Kay</a>, <a href="/search/nucl-ex?searchtype=author&query=Freeman%2C+S+J">S. J. Freeman</a>, <a href="/search/nucl-ex?searchtype=author&query=Schiffer%2C+J+P">J. P. Schiffer</a>, <a href="/search/nucl-ex?searchtype=author&query=Clark%2C+J+A">J. A. Clark</a>, <a href="/search/nucl-ex?searchtype=author&query=Deibel%2C+C">C. Deibel</a>, <a href="/search/nucl-ex?searchtype=author&query=Heinz%2C+A">A. Heinz</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Wrede%2C+C">C. Wrede</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="0709.0468v1-abstract-short" style="display: inline;"> The behaviour of the i13/2 and h9/2 single-neutron strength was studied with the (4He,3He) reaction on 138Ba, 140Ce, 142Nd and 144Sm targets at a beam energy of 51 MeV. The separation between the single-neutron states i13/2 and h9/2 was measured in N =83 nuclei with changing proton number. To this end spectroscopic factors for states populated in high-l transfer were extracted from the data. Som… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0709.0468v1-abstract-full').style.display = 'inline'; document.getElementById('0709.0468v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0709.0468v1-abstract-full" style="display: none;"> The behaviour of the i13/2 and h9/2 single-neutron strength was studied with the (4He,3He) reaction on 138Ba, 140Ce, 142Nd and 144Sm targets at a beam energy of 51 MeV. The separation between the single-neutron states i13/2 and h9/2 was measured in N =83 nuclei with changing proton number. To this end spectroscopic factors for states populated in high-l transfer were extracted from the data. Some mixing of l=5 and 6 strength was observed with states that are formed by coupling the f7/2 state to the 2+ and 3- vibrational states and the mixing matrix elements were found to be remarkably constant. The centroids of the strength indicate a systematic change in the energies of the i13/2 and h9/2 single-neutron states with increasing proton number that is in quantitative agreement with the effects expected from the tensor interaction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0709.0468v1-abstract-full').style.display = 'none'; document.getElementById('0709.0468v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 September, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages of text, 3 diagrams</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Lett.B658:216-221,2008 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/nucl-ex/0701003">arXiv:nucl-ex/0701003</a> <span> [<a href="https://arxiv.org/pdf/nucl-ex/0701003">pdf</a>, <a href="https://arxiv.org/format/nucl-ex/0701003">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.75.051301">10.1103/PhysRevC.75.051301 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Pair correlations in nuclei involved in neutrinoless double beta decay: 76Ge and 76Se </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Freeman%2C+S+J">S. J. Freeman</a>, <a href="/search/nucl-ex?searchtype=author&query=Schiffer%2C+J+P">J. P. Schiffer</a>, <a href="/search/nucl-ex?searchtype=author&query=Villari%2C+A+C+C">A. C. C. Villari</a>, <a href="/search/nucl-ex?searchtype=author&query=Clark%2C+J+A">J. A. Clark</a>, <a href="/search/nucl-ex?searchtype=author&query=Deibel%2C+C">C. Deibel</a>, <a href="/search/nucl-ex?searchtype=author&query=Gros%2C+S">S. Gros</a>, <a href="/search/nucl-ex?searchtype=author&query=Heinz%2C+A">A. Heinz</a>, <a href="/search/nucl-ex?searchtype=author&query=Hirata%2C+D">D. Hirata</a>, <a href="/search/nucl-ex?searchtype=author&query=Jiang%2C+C+L">C. L. Jiang</a>, <a href="/search/nucl-ex?searchtype=author&query=Kay%2C+B+P">B. P. Kay</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Parker%2C+P+D">P. D. Parker</a>, <a href="/search/nucl-ex?searchtype=author&query=Qian%2C+J">J. Qian</a>, <a href="/search/nucl-ex?searchtype=author&query=Rehm%2C+K+E">K. E. Rehm</a>, <a href="/search/nucl-ex?searchtype=author&query=Tang%2C+X+D">X. D. Tang</a>, <a href="/search/nucl-ex?searchtype=author&query=Werner%2C+V">V. Werner</a>, <a href="/search/nucl-ex?searchtype=author&query=Wrede%2C+C">C. Wrede</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="nucl-ex/0701003v2-abstract-short" style="display: inline;"> Precision measurements were carried out to test the similarities between the ground states of 76Ge and 76Se. The extent to which these two nuclei can be characterized as consisting of correlated pairs of neutrons in a BCS-like ground state was studied. The pair removal (p,t) reaction was measured at the far forward angle of 3 degrees. The relative cross sections are consistent (at the 5% level)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0701003v2-abstract-full').style.display = 'inline'; document.getElementById('nucl-ex/0701003v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="nucl-ex/0701003v2-abstract-full" style="display: none;"> Precision measurements were carried out to test the similarities between the ground states of 76Ge and 76Se. The extent to which these two nuclei can be characterized as consisting of correlated pairs of neutrons in a BCS-like ground state was studied. The pair removal (p,t) reaction was measured at the far forward angle of 3 degrees. The relative cross sections are consistent (at the 5% level) with the description of these nuclei in terms of a correlated pairing state outside the N=28 closed shells with no pairing vibrations. Data were also obtained for 74Ge and 78Se. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0701003v2-abstract-full').style.display = 'none'; document.getElementById('nucl-ex/0701003v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 March, 2007; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 January, 2007; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2007. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.C75:051301,2007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/nucl-ex/0308008">arXiv:nucl-ex/0308008</a> <span> [<a href="https://arxiv.org/pdf/nucl-ex/0308008">pdf</a>, <a href="https://arxiv.org/ps/nucl-ex/0308008">ps</a>, <a href="https://arxiv.org/format/nucl-ex/0308008">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevC.69.048801">10.1103/PhysRevC.69.048801 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Particle decay branching ratios for states of astrophysical importance in 19Ne </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/nucl-ex?searchtype=author&query=Visser%2C+D+W">D. W. Visser</a>, <a href="/search/nucl-ex?searchtype=author&query=Caggiano%2C+J+A">J. A. Caggiano</a>, <a href="/search/nucl-ex?searchtype=author&query=Lewis%2C+R">R. Lewis</a>, <a href="/search/nucl-ex?searchtype=author&query=Handler%2C+W+B">W. B. Handler</a>, <a href="/search/nucl-ex?searchtype=author&query=Parikh%2C+A">A. Parikh</a>, <a href="/search/nucl-ex?searchtype=author&query=Parker%2C+P+D">P. D. Parker</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="nucl-ex/0308008v3-abstract-short" style="display: inline;"> We have measured proton and alpha-particle branching ratios of excited states in 19Ne formed using the 19F(3He,t) reaction at a beam energy of 25 MeV. These ratios have a large impact on the astrophysical reaction rates of 15O(alpha,gamma), 18F(p,gamma) and 18F(p,alpha), which are of interest in understanding energy generation in x-ray bursts and in interpreting anticipated gamma-ray observation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0308008v3-abstract-full').style.display = 'inline'; document.getElementById('nucl-ex/0308008v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="nucl-ex/0308008v3-abstract-full" style="display: none;"> We have measured proton and alpha-particle branching ratios of excited states in 19Ne formed using the 19F(3He,t) reaction at a beam energy of 25 MeV. These ratios have a large impact on the astrophysical reaction rates of 15O(alpha,gamma), 18F(p,gamma) and 18F(p,alpha), which are of interest in understanding energy generation in x-ray bursts and in interpreting anticipated gamma-ray observations of novae. We detect decay protons and alpha-particles using a silicon detector array in coincidence with tritons measured in the focal plane detector of our Enge split-pole spectrograph. The silicon array consists of five strip detectors of the type used in the Louvain-Edinburgh Detector Array, subtending angles from 130 degrees to 165 degrees with approximately 14% lab efficiency. The correlation angular distributions give additional confidence in some prior spin-parity assignments that were based on gamma branchings. We measure Gamma_p/Gamma=0.387+-0.016 for the 665 keV proton resonance, which agrees well with the direct measurement of Bardayan et al. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('nucl-ex/0308008v3-abstract-full').style.display = 'none'; document.getElementById('nucl-ex/0308008v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 February, 2004; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 August, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2003. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 2 figures, 3 tables. Prepared using RevTex 4 and BibTex. Further minor revisions, incl. fig. 1 font size increase, 1 table removal, and minor changes to the text</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev. C69 (2004) 048801 </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div>   <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/license/index.html">Copyright</a></li> <li><a href="https://info.arxiv.org/help/policies/privacy_policy.html">Privacy Policy</a></li> </ul> </div> <div class="column sorry-app-links"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/help/web_accessibility.html">Web Accessibility Assistance</a></li> <li> <p class="help"> <a class="a11y-main-link" href="https://status.arxiv.org" target="_blank">arXiv Operational Status <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 256 512" class="icon filter-dark_grey" role="presentation"><path d="M224.3 273l-136 136c-9.4 9.4-24.6 9.4-33.9 0l-22.6-22.6c-9.4-9.4-9.4-24.6 0-33.9l96.4-96.4-96.4-96.4c-9.4-9.4-9.4-24.6 0-33.9L54.3 103c9.4-9.4 24.6-9.4 33.9 0l136 136c9.5 9.4 9.5 24.6.1 34z"/></svg></a><br> Get status notifications via <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/email/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg>email</a> or <a class="is-link" href="https://subscribe.sorryapp.com/24846f03/slack/new" target="_blank"><svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 448 512" class="icon filter-black" role="presentation"><path d="M94.12 315.1c0 25.9-21.16 47.06-47.06 47.06S0 341 0 315.1c0-25.9 21.16-47.06 47.06-47.06h47.06v47.06zm23.72 0c0-25.9 21.16-47.06 47.06-47.06s47.06 21.16 47.06 47.06v117.84c0 25.9-21.16 47.06-47.06 47.06s-47.06-21.16-47.06-47.06V315.1zm47.06-188.98c-25.9 0-47.06-21.16-47.06-47.06S139 32 164.9 32s47.06 21.16 47.06 47.06v47.06H164.9zm0 23.72c25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06H47.06C21.16 243.96 0 222.8 0 196.9s21.16-47.06 47.06-47.06H164.9zm188.98 47.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06s-21.16 47.06-47.06 47.06h-47.06V196.9zm-23.72 0c0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06V79.06c0-25.9 21.16-47.06 47.06-47.06 25.9 0 47.06 21.16 47.06 47.06V196.9zM283.1 385.88c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06-25.9 0-47.06-21.16-47.06-47.06v-47.06h47.06zm0-23.72c-25.9 0-47.06-21.16-47.06-47.06 0-25.9 21.16-47.06 47.06-47.06h117.84c25.9 0 47.06 21.16 47.06 47.06 0 25.9-21.16 47.06-47.06 47.06H283.1z"/></svg>slack</a> </p> </li> </ul> </div> </div> </div>  </div> </footer> <script src="https://static.arxiv.org/static/base/1.0.0a5/js/member_acknowledgement.js"></script> </body> </html>

CINXE.COM

Search | arXiv e-print repository