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 1–41 of 41 results for author: <span class="mathjax">Matsuda, S</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/" aria-role="search"> <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="Matsuda, S"> </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=Matsuda%2C+S&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="Matsuda, S"> <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/2501.04107">arXiv:2501.04107</a> <span> [<a href="https://arxiv.org/pdf/2501.04107">pdf</a>, <a href="https://arxiv.org/format/2501.04107">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Geophysics">physics.geo-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-ph</span> </div> </div> <p class="title is-5 mathjax"> A Characteristic Signature of Magnetospheric Wave-Particle Interactions Found in the Turbulent E-region </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ivarsen%2C+M+F">Magnus F Ivarsen</a>, <a href="/search/?searchtype=author&query=Miyashita%2C+Y">Yukinaga Miyashita</a>, <a href="/search/?searchtype=author&query=St-Maurice%2C+J">Jean-Pierre St-Maurice</a>, <a href="/search/?searchtype=author&query=Hussey%2C+G+C">Glenn C Hussey</a>, <a href="/search/?searchtype=author&query=Pitzel%2C+B">Brian Pitzel</a>, <a href="/search/?searchtype=author&query=Galeschuk%2C+D">Draven Galeschuk</a>, <a href="/search/?searchtype=author&query=Marei%2C+S">Saif Marei</a>, <a href="/search/?searchtype=author&query=Horne%2C+R+B">Richard B Horne</a>, <a href="/search/?searchtype=author&query=Kasahara%2C+Y">Yoshiya Kasahara</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">Shoya Matsuda</a>, <a href="/search/?searchtype=author&query=Kasahara%2C+S">Satoshi Kasahara</a>, <a href="/search/?searchtype=author&query=Keika%2C+K">Kunihiro Keika</a>, <a href="/search/?searchtype=author&query=Miyoshi%2C+Y">Yoshizumi Miyoshi</a>, <a href="/search/?searchtype=author&query=Yamamoto%2C+K">Kazuhiro Yamamoto</a>, <a href="/search/?searchtype=author&query=Shinbori%2C+A">Atsuki Shinbori</a>, <a href="/search/?searchtype=author&query=Huyghebaert%2C+D+R">Devin R Huyghebaert</a>, <a href="/search/?searchtype=author&query=Matsuoka%2C+A">Ayako Matsuoka</a>, <a href="/search/?searchtype=author&query=Yokota%2C+S">Shoichiro Yokota</a>, <a href="/search/?searchtype=author&query=Tsuchiya%2C+F">Fuminori Tsuchiya</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="2501.04107v1-abstract-short" style="display: inline;"> Electromagnetic waves in the magnetosphere scatter electrons, causing them to precipitate deep into Earth's atmosphere, where they impart their temporal characteristics to diffuse aurorae. Using radar-observations of the ionospheric E-region and satellite observations from the magnetosphere, we demonstrate a close and unprecedented association between enhanced electrostatic cyclotron harmonic wave… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.04107v1-abstract-full').style.display = 'inline'; document.getElementById('2501.04107v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.04107v1-abstract-full" style="display: none;"> Electromagnetic waves in the magnetosphere scatter electrons, causing them to precipitate deep into Earth's atmosphere, where they impart their temporal characteristics to diffuse aurorae. Using radar-observations of the ionospheric E-region and satellite observations from the magnetosphere, we demonstrate a close and unprecedented association between enhanced electrostatic cyclotron harmonic wave activity in the magnetosphere and the appearance of meter-scale ionospheric plasma turbulence observed a few seconds later in the lower ionosphere on nearby magnetic field lines. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.04107v1-abstract-full').style.display = 'none'; document.getElementById('2501.04107v1-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> 7 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </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">10 pages, 6 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/2409.09900">arXiv:2409.09900</a> <span> [<a href="https://arxiv.org/pdf/2409.09900">pdf</a>, <a href="https://arxiv.org/format/2409.09900">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Plasma Physics">physics.plasm-ph</span> </div> </div> <p class="title is-5 mathjax"> Variation of Whistler-Mode Wave Characteristics Along Magnetic Field Lines: Comparison of Near-Equatorial THEMIS and Middle-Latitude ERG Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kadan%2C+S">Sophie Kadan</a>, <a href="/search/?searchtype=author&query=Zhang%2C+X">Xiao-Jia Zhang</a>, <a href="/search/?searchtype=author&query=Artemyev%2C+A">Anton Artemyev</a>, <a href="/search/?searchtype=author&query=Miyoshi%2C+Y">Yoshizumi Miyoshi</a>, <a href="/search/?searchtype=author&query=Matsuoka%2C+A">Ayako Matsuoka</a>, <a href="/search/?searchtype=author&query=Kasahara%2C+Y">Yoshiya Kasahara</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">Shoya Matsuda</a>, <a href="/search/?searchtype=author&query=Hori%2C+T">Tomoaki Hori</a>, <a href="/search/?searchtype=author&query=Teramoto%2C+M">Mariko Teramoto</a>, <a href="/search/?searchtype=author&query=Yamamoto%2C+K">Kazuhiro Yamamoto</a>, <a href="/search/?searchtype=author&query=Shinohara%2C+I">Iku Shinohara</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="2409.09900v1-abstract-short" style="display: inline;"> The latitudinal distribution of whistler-mode wave intensity plays a crucial role in determining the efficiency and energy of electrons scattered by these waves in the outer radiation belt. Traditionally, this wave property has mostly been derived from statistical measurements of off-equatorial spacecraft, which collect intensity data at various latitudes under different geomagnetic conditions and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.09900v1-abstract-full').style.display = 'inline'; document.getElementById('2409.09900v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.09900v1-abstract-full" style="display: none;"> The latitudinal distribution of whistler-mode wave intensity plays a crucial role in determining the efficiency and energy of electrons scattered by these waves in the outer radiation belt. Traditionally, this wave property has mostly been derived from statistical measurements of off-equatorial spacecraft, which collect intensity data at various latitudes under different geomagnetic conditions and at different times. In this study we examine a set of events captured by both the near-equatorial THEMIS spacecraft and the off-equatorial ERG spacecraft. Specifically, we compare the whistler-mode wave intensity from THEMIS and ERG measurements at the same MLT and time sectors. Similar wave spectrum characteristics confirm that THEMIS and ERG indeed observed the same wave activity. However, upon closer examination of the wave intensity variations, we identify two distinct categories of events: those that follow the statistically predicted variations in wave intensity along magnetic latitudes, and those that exhibit rapid wave intensity decay away from the equatorial plane. We analyze main characteristics of events from both categories and discuss possible implications of our analysis for radiation belt models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.09900v1-abstract-full').style.display = 'none'; document.getElementById('2409.09900v1-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> 15 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.18335">arXiv:2406.18335</a> <span> [<a href="https://arxiv.org/pdf/2406.18335">pdf</a>, <a href="https://arxiv.org/format/2406.18335">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</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"> New high-precision measurement system for electron-positron pairs from sub-GeV/GeV gamma-rays in the emulsion telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Nakamura%2C+Y">Yuya Nakamura</a>, <a href="/search/?searchtype=author&query=Aoki%2C+S">Shigeki Aoki</a>, <a href="/search/?searchtype=author&query=Hayakawa%2C+T">Tomohiro Hayakawa</a>, <a href="/search/?searchtype=author&query=Iyono%2C+A">Atsushi Iyono</a>, <a href="/search/?searchtype=author&query=Karasuno%2C+A">Ayaka Karasuno</a>, <a href="/search/?searchtype=author&query=Kodama%2C+K">Kohichi Kodama</a>, <a href="/search/?searchtype=author&query=Komatani%2C+R">Ryosuke Komatani</a>, <a href="/search/?searchtype=author&query=Komatsu%2C+M">Masahiro Komatsu</a>, <a href="/search/?searchtype=author&query=Komiyama%2C+M">Masahiro Komiyama</a>, <a href="/search/?searchtype=author&query=Kuretsubo%2C+K">Kenji Kuretsubo</a>, <a href="/search/?searchtype=author&query=Marushima%2C+T">Toshitsugu Marushima</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">Syota Matsuda</a>, <a href="/search/?searchtype=author&query=Morishima%2C+K">Kunihiro Morishima</a>, <a href="/search/?searchtype=author&query=Morishita%2C+M">Misaki Morishita</a>, <a href="/search/?searchtype=author&query=Naganawa%2C+N">Naotaka Naganawa</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+M">Mitsuhiro Nakamura</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+M">Motoya Nakamura</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+T">Takafumi Nakamura</a>, <a href="/search/?searchtype=author&query=Nakano%2C+N">Noboru Nakano</a>, <a href="/search/?searchtype=author&query=Nakano%2C+T">Toshiyuki Nakano</a>, <a href="/search/?searchtype=author&query=Nishio%2C+A">Akira Nishio</a>, <a href="/search/?searchtype=author&query=Oda%2C+M">Miyuki Oda</a>, <a href="/search/?searchtype=author&query=Rokujo%2C+H">Hiroki Rokujo</a>, <a href="/search/?searchtype=author&query=Sato%2C+O">Osamu Sato</a>, <a href="/search/?searchtype=author&query=Sugimura%2C+K">Kou Sugimura</a> , et al. (5 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="2406.18335v1-abstract-short" style="display: inline;"> The GRAINE project observes cosmic gamma-rays, using a balloon-borne emulsion-film-based telescope in the sub-GeV/GeV energy band. We reported in our previous balloon experiment in 2018, GRAINE2018, the detection of the known brightest source, Vela pulsar, with the highest angular resolution ever reported in an energy range of $>$80 MeV. However, the emulsion scanning system used in the experiment… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.18335v1-abstract-full').style.display = 'inline'; document.getElementById('2406.18335v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.18335v1-abstract-full" style="display: none;"> The GRAINE project observes cosmic gamma-rays, using a balloon-borne emulsion-film-based telescope in the sub-GeV/GeV energy band. We reported in our previous balloon experiment in 2018, GRAINE2018, the detection of the known brightest source, Vela pulsar, with the highest angular resolution ever reported in an energy range of $>$80 MeV. However, the emulsion scanning system used in the experiment was designed to achieve a high-speed scanning, and it was not accurate enough to ensure the optimum spacial resolution of the emulsion film and limited the performance. Here, we report a new high-precision scanning system that can be used to greatly improve the observation result of GRAINE2018 and also be employed in future experiments. The system involves a new algorithm that recognizes each silver grain on an emulsion film and is capable of measuring tracks with a positional resolution for the passing points of tracks of almost the same as the intrinsic resolution of nuclear emulsion film ($\sim$70 nm). This resolution is approximately one order of magnitude smaller than that obtained with the high-speed scanning system. With this system, an angular resolution for gamma-rays of 0.1$^\circ$ at 1 GeV is expected to be achieved. Furthermore, we successfully combine the new high-precision system with the existing high-speed system, establishing the system to make a high-speed and high-precision measurement. Employing these systems, we reanalyze the gamma-ray events detected previously by only the high-speed system in GRAINE2018 and obtain an about three times higher angular resolution (0.22$^\circ$) in 500--700 MeV than the original value. The high-resolution observation may bring new insights into the gamma-ray emission from the Galactic center region and may realize polarization measurements of high-energy cosmic gamma-rays. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.18335v1-abstract-full').style.display = 'none'; document.getElementById('2406.18335v1-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </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">20 pages, 11 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/2304.13927">arXiv:2304.13927</a> <span> [<a href="https://arxiv.org/pdf/2304.13927">pdf</a>, <a href="https://arxiv.org/ps/2304.13927">ps</a>, <a href="https://arxiv.org/format/2304.13927">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Materials Science">cond-mat.mtrl-sci</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Artificial Intelligence">cs.AI</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Robotics">cs.RO</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/10.1080/27660400.2023.2232297">10.1080/27660400.2023.2232297 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NIMS-OS: An automation software to implement a closed loop between artificial intelligence and robotic experiments in materials science </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Tamura%2C+R">Ryo Tamura</a>, <a href="/search/?searchtype=author&query=Tsuda%2C+K">Koji Tsuda</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">Shoichi Matsuda</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="2304.13927v1-abstract-short" style="display: inline;"> NIMS-OS (NIMS Orchestration System) is a Python library created to realize a closed loop of robotic experiments and artificial intelligence (AI) without human intervention for automated materials exploration. It uses various combinations of modules to operate autonomously. Each module acts as an AI for materials exploration or a controller for a robotic experiments. As AI techniques, Bayesian opti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.13927v1-abstract-full').style.display = 'inline'; document.getElementById('2304.13927v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.13927v1-abstract-full" style="display: none;"> NIMS-OS (NIMS Orchestration System) is a Python library created to realize a closed loop of robotic experiments and artificial intelligence (AI) without human intervention for automated materials exploration. It uses various combinations of modules to operate autonomously. Each module acts as an AI for materials exploration or a controller for a robotic experiments. As AI techniques, Bayesian optimization (PHYSBO), boundless objective-free exploration (BLOX), phase diagram construction (PDC), and random exploration (RE) methods can be used. Moreover, a system called NIMS automated robotic electrochemical experiments (NAREE) is available as a set of robotic experimental equipment. Visualization tools for the results are also included, which allows users to check the optimization results in real time. Newly created modules for AI and robotic experiments can be added easily to extend the functionality of the system. In addition, we developed a GUI application to control NIMS-OS.To demonstrate the operation of NIMS-OS, we consider an automated exploration for new electrolytes. NIMS-OS is available at https://github.com/nimsos-dev/nimsos. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.13927v1-abstract-full').style.display = 'none'; document.getElementById('2304.13927v1-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </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">29 pages, 5 figures, 2 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Science and Technology of Advanced Materials: Methods 3, 1, 2232297 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.10348">arXiv:2203.10348</a> <span> [<a href="https://arxiv.org/pdf/2203.10348">pdf</a>, <a href="https://arxiv.org/format/2203.10348">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Computer Vision and Pattern Recognition">cs.CV</span> </div> </div> <p class="title is-5 mathjax"> Font Generation with Missing Impression Labels </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Matsuda%2C+S">Seiya Matsuda</a>, <a href="/search/?searchtype=author&query=Kimura%2C+A">Akisato Kimura</a>, <a href="/search/?searchtype=author&query=Uchida%2C+S">Seiichi Uchida</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="2203.10348v2-abstract-short" style="display: inline;"> Our goal is to generate fonts with specific impressions, by training a generative adversarial network with a font dataset with impression labels. The main difficulty is that font impression is ambiguous and the absence of an impression label does not always mean that the font does not have the impression. This paper proposes a font generation model that is robust against missing impression labels.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.10348v2-abstract-full').style.display = 'inline'; document.getElementById('2203.10348v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.10348v2-abstract-full" style="display: none;"> Our goal is to generate fonts with specific impressions, by training a generative adversarial network with a font dataset with impression labels. The main difficulty is that font impression is ambiguous and the absence of an impression label does not always mean that the font does not have the impression. This paper proposes a font generation model that is robust against missing impression labels. The key ideas of the proposed method are (1)a co-occurrence-based missing label estimator and (2)an impression label space compressor. The first is to interpolate missing impression labels based on the co-occurrence of labels in the dataset and use them for training the model as completed label conditions. The second is an encoder-decoder module to compress the high-dimensional impression space into low-dimensional. We proved that the proposed model generates high-quality font images using multi-label data with missing labels through qualitative and quantitative evaluations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.10348v2-abstract-full').style.display = 'none'; document.getElementById('2203.10348v2-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> 2 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">Accepted ICPR2022</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.10452">arXiv:2104.10452</a> <span> [<a href="https://arxiv.org/pdf/2104.10452">pdf</a>, <a href="https://arxiv.org/format/2104.10452">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</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/10.1088/1748-0221/16/08/p08023">10.1088/1748-0221/16/08/p08023 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The nylon balloon for xenon loaded liquid scintillator in KamLAND-Zen 800 neutrinoless double-beta decay search experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=collaboration%2C+K">KamLAND-Zen collaboration</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Hosokawa%2C+K">K. Hosokawa</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Nakada%2C+T">T. Nakada</a>, <a href="/search/?searchtype=author&query=Obara%2C+S">S. Obara</a>, <a href="/search/?searchtype=author&query=Ozaki%2C+H">H. Ozaki</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a>, <a href="/search/?searchtype=author&query=Watanabe%2C+H">H. Watanabe</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Hata%2C+K">K. Hata</a>, <a href="/search/?searchtype=author&query=Hayashi%2C+A">A. Hayashi</a>, <a href="/search/?searchtype=author&query=Honda%2C+Y">Y. Honda</a>, <a href="/search/?searchtype=author&query=Ieki%2C+S">S. Ieki</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Ishikawa%2C+S">S. Ishikawa</a>, <a href="/search/?searchtype=author&query=Kamei%2C+Y">Y. Kamei</a>, <a href="/search/?searchtype=author&query=Kamizawa%2C+K">K. Kamizawa</a> , et al. (49 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="2104.10452v3-abstract-short" style="display: inline;"> The KamLAND-Zen 800 experiment is searching for the neutrinoless double-beta decay of $^{136}$Xe by using $^{136}$Xe-loaded liquid scintillator. The liquid scintillator is enclosed inside a balloon made of thin, transparent, low-radioactivity film that we call Inner Balloon (IB). The IB, apart from guaranteeing the liquid containment, also allows to minimize the background from cosmogenic muon-spa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.10452v3-abstract-full').style.display = 'inline'; document.getElementById('2104.10452v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.10452v3-abstract-full" style="display: none;"> The KamLAND-Zen 800 experiment is searching for the neutrinoless double-beta decay of $^{136}$Xe by using $^{136}$Xe-loaded liquid scintillator. The liquid scintillator is enclosed inside a balloon made of thin, transparent, low-radioactivity film that we call Inner Balloon (IB). The IB, apart from guaranteeing the liquid containment, also allows to minimize the background from cosmogenic muon-spallation products and $^{8}$B solar neutrinos. Indeed these events could contribute to the total counts in the region of interest around the Q-value of the double-beta decay of $^{136}$Xe. In this paper, we present an overview of the IB and describe the various steps of its commissioning minimizing the radioactive contaminations, from the material selection, to the fabrication of the balloon and its installation inside the KamLAND detector. Finally, we show the impact of the IB on the KamLAND background as measured by the KamLAND detector itself. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.10452v3-abstract-full').style.display = 'none'; document.getElementById('2104.10452v3-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 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">23 pages, 16 figures, to be submitted to JINST</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2021 JINST 16 P08023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.12347">arXiv:2103.12347</a> <span> [<a href="https://arxiv.org/pdf/2103.12347">pdf</a>, <a href="https://arxiv.org/format/2103.12347">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Computer Vision and Pattern Recognition">cs.CV</span> </div> </div> <p class="title is-5 mathjax"> Shared Latent Space of Font Shapes and Their Noisy Impressions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kang%2C+J">Jihun Kang</a>, <a href="/search/?searchtype=author&query=Haraguchi%2C+D">Daichi Haraguchi</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">Seiya Matsuda</a>, <a href="/search/?searchtype=author&query=Kimura%2C+A">Akisato Kimura</a>, <a href="/search/?searchtype=author&query=Uchida%2C+S">Seiichi Uchida</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="2103.12347v3-abstract-short" style="display: inline;"> Styles of typefaces or fonts are often associated with specific impressions, such as heavy, contemporary, or elegant. This indicates that there are certain correlations between font shapes and their impressions. To understand the correlations, this paper realizes a shared latent space where a font and its impressions are embedded nearby. The difficulty is that the impression words attached to a fo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.12347v3-abstract-full').style.display = 'inline'; document.getElementById('2103.12347v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.12347v3-abstract-full" style="display: none;"> Styles of typefaces or fonts are often associated with specific impressions, such as heavy, contemporary, or elegant. This indicates that there are certain correlations between font shapes and their impressions. To understand the correlations, this paper realizes a shared latent space where a font and its impressions are embedded nearby. The difficulty is that the impression words attached to a font are often very noisy. This is because impression words are very subjective and diverse. More importantly, some impression words have no direct relevance to the font shapes and will disturb the realization of the shared latent space. We, therefore, use DeepSets for enhancing shape-relevant words and suppressing shape irrelevant words automatically while training the shared latent space. Quantitative and qualitative experimental results with a large-scale font-impression dataset demonstrate that the shared latent space by the proposed method describes the correlation appropriately, especially for the shape-relevant impression words. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.12347v3-abstract-full').style.display = 'none'; document.getElementById('2103.12347v3-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> 2 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 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">accepted at MMM2022</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.10036">arXiv:2103.10036</a> <span> [<a href="https://arxiv.org/pdf/2103.10036">pdf</a>, <a href="https://arxiv.org/format/2103.10036">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Computer Vision and Pattern Recognition">cs.CV</span> </div> </div> <p class="title is-5 mathjax"> Impressions2Font: Generating Fonts by Specifying Impressions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Matsuda%2C+S">Seiya Matsuda</a>, <a href="/search/?searchtype=author&query=Kimura%2C+A">Akisato Kimura</a>, <a href="/search/?searchtype=author&query=Uchida%2C+S">Seiichi Uchida</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="2103.10036v2-abstract-short" style="display: inline;"> Various fonts give us various impressions, which are often represented by words. This paper proposes Impressions2Font (Imp2Font) that generates font images with specific impressions. Imp2Font is an extended version of conditional generative adversarial networks (GANs). More precisely, Imp2Font accepts an arbitrary number of impression words as the condition to generate the font images. These impre… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.10036v2-abstract-full').style.display = 'inline'; document.getElementById('2103.10036v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.10036v2-abstract-full" style="display: none;"> Various fonts give us various impressions, which are often represented by words. This paper proposes Impressions2Font (Imp2Font) that generates font images with specific impressions. Imp2Font is an extended version of conditional generative adversarial networks (GANs). More precisely, Imp2Font accepts an arbitrary number of impression words as the condition to generate the font images. These impression words are converted into a soft-constraint vector by an impression embedding module built on a word embedding technique. Qualitative and quantitative evaluations prove that Imp2Font generates font images with higher quality than comparative methods by providing multiple impression words or even unlearned words. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.10036v2-abstract-full').style.display = 'none'; document.getElementById('2103.10036v2-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> 21 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 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">accepted at ICDAR2021</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.04489">arXiv:2010.04489</a> <span> [<a href="https://arxiv.org/pdf/2010.04489">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Chemical Physics">physics.chem-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Applied Physics">physics.app-ph</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/10.35848/1347-4065/abf4a1">10.35848/1347-4065/abf4a1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Non-destructive visualization of short circuits in lithium-ion batteries by magnetic field imaging system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Suzuki%2C+S">Shogo Suzuki</a>, <a href="/search/?searchtype=author&query=Okada%2C+H">Hideaki Okada</a>, <a href="/search/?searchtype=author&query=Yabumoto%2C+K">Kai Yabumoto</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">Seiju Matsuda</a>, <a href="/search/?searchtype=author&query=Mima%2C+Y">Yuki Mima</a>, <a href="/search/?searchtype=author&query=Kimura%2C+N">Noriaki Kimura</a>, <a href="/search/?searchtype=author&query=Kimura%2C+K">Kenjiro Kimura</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="2010.04489v1-abstract-short" style="display: inline;"> To develop a high-density and long-life lithium-ion battery, a technology is needed that allows non-destructive visualization of the spatial distribution of deteriorated parts after cycle test. In the present study, we measured the distribution of the magnetic field leaking from the lithium-ion battery during its operation. Based on the measurement results, we evaluated the current density distrib… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.04489v1-abstract-full').style.display = 'inline'; document.getElementById('2010.04489v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.04489v1-abstract-full" style="display: none;"> To develop a high-density and long-life lithium-ion battery, a technology is needed that allows non-destructive visualization of the spatial distribution of deteriorated parts after cycle test. In the present study, we measured the distribution of the magnetic field leaking from the lithium-ion battery during its operation. Based on the measurement results, we evaluated the current density distribution inside a battery using the electric current reconstruction process. With respect to the changes in an internal state of the lithium-ion battery associated with cycle deterioration, we successfully visualized the spatial changes in the conductivity distribution inside the lithium-ion battery. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.04489v1-abstract-full').style.display = 'none'; document.getElementById('2010.04489v1-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </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">11 pages, 5 figures, letter</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1611.05527">arXiv:1611.05527</a> <span> [<a href="https://arxiv.org/pdf/1611.05527">pdf</a>, <a href="https://arxiv.org/ps/1611.05527">ps</a>, <a href="https://arxiv.org/format/1611.05527">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Computation and Language">cs.CL</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">cs.LG</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">stat.ML</span> </div> </div> <p class="title is-5 mathjax"> Automatic Node Selection for Deep Neural Networks using Group Lasso Regularization </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ochiai%2C+T">Tsubasa Ochiai</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">Shigeki Matsuda</a>, <a href="/search/?searchtype=author&query=Watanabe%2C+H">Hideyuki Watanabe</a>, <a href="/search/?searchtype=author&query=Katagiri%2C+S">Shigeru Katagiri</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="1611.05527v1-abstract-short" style="display: inline;"> We examine the effect of the Group Lasso (gLasso) regularizer in selecting the salient nodes of Deep Neural Network (DNN) hidden layers by applying a DNN-HMM hybrid speech recognizer to TED Talks speech data. We test two types of gLasso regularization, one for outgoing weight vectors and another for incoming weight vectors, as well as two sizes of DNNs: 2048 hidden layer nodes and 4096 nodes. Furt… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.05527v1-abstract-full').style.display = 'inline'; document.getElementById('1611.05527v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.05527v1-abstract-full" style="display: none;"> We examine the effect of the Group Lasso (gLasso) regularizer in selecting the salient nodes of Deep Neural Network (DNN) hidden layers by applying a DNN-HMM hybrid speech recognizer to TED Talks speech data. We test two types of gLasso regularization, one for outgoing weight vectors and another for incoming weight vectors, as well as two sizes of DNNs: 2048 hidden layer nodes and 4096 nodes. Furthermore, we compare gLasso and L2 regularizers. Our experiment results demonstrate that our DNN training, in which the gLasso regularizer was embedded, successfully selected the hidden layer nodes that are necessary and sufficient for achieving high classification power. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.05527v1-abstract-full').style.display = 'none'; document.getElementById('1611.05527v1-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 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2016. </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">Submitted to ICASSP 2017</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1606.07155">arXiv:1606.07155</a> <span> [<a href="https://arxiv.org/pdf/1606.07155">pdf</a>, <a href="https://arxiv.org/ps/1606.07155">ps</a>, <a href="https://arxiv.org/format/1606.07155">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="High Energy Physics - Experiment">hep-ex</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/10.3847/2041-8205/829/2/L34">10.3847/2041-8205/829/2/L34 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for electron antineutrinos associated with gravitational wave events GW150914 and GW151226 using KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=KamLAND+Collaboration"> KamLAND Collaboration</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hayashi%2C+A">A. Hayashi</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Karino%2C+Y">Y. Karino</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Obara%2C+S">S. Obara</a>, <a href="/search/?searchtype=author&query=Oura%2C+T">T. Oura</a>, <a href="/search/?searchtype=author&query=Ozaki%2C+H">H. Ozaki</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/?searchtype=author&query=Shirahata%2C+Y">Y. Shirahata</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/?searchtype=author&query=Takai%2C+T">T. Takai</a>, <a href="/search/?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/?searchtype=author&query=Teraoka%2C+Y">Y. Teraoka</a>, <a href="/search/?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a> , et al. (23 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="1606.07155v2-abstract-short" style="display: inline;"> We present a search for low energy antineutrino events coincident with the gravitational wave events GW150914 and GW151226, and the candidate event LVT151012 using KamLAND, a kiloton-scale antineutrino detector. We find no inverse beta-decay neutrino events within $\pm 500$ seconds of either gravitational wave signal. This non-detection is used to constrain the electron antineutrino fluence and th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.07155v2-abstract-full').style.display = 'inline'; document.getElementById('1606.07155v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1606.07155v2-abstract-full" style="display: none;"> We present a search for low energy antineutrino events coincident with the gravitational wave events GW150914 and GW151226, and the candidate event LVT151012 using KamLAND, a kiloton-scale antineutrino detector. We find no inverse beta-decay neutrino events within $\pm 500$ seconds of either gravitational wave signal. This non-detection is used to constrain the electron antineutrino fluence and the luminosity of the astrophysical sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1606.07155v2-abstract-full').style.display = 'none'; document.getElementById('1606.07155v2-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, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 June, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2016. </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">11 pages, 4 figures, as published in ApJL. Updated to replace power law spectrum with Fermi Dirac spectrum</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astrophys.J.829, L34, 2016 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1509.09043">arXiv:1509.09043</a> <span> [<a href="https://arxiv.org/pdf/1509.09043">pdf</a>, <a href="https://arxiv.org/ps/1509.09043">ps</a>, <a href="https://arxiv.org/format/1509.09043">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Materials Science">cond-mat.mtrl-sci</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/10.7566/JPSJ.84.114712">10.7566/JPSJ.84.114712 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Structural Domain Switching by Magnetic Fields in RAl$_3$C$_3$ (R=Rare Earth) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Matsumura%2C+T">T. Matsumura</a>, <a href="/search/?searchtype=author&query=Hayashi%2C+Y">Y. Hayashi</a>, <a href="/search/?searchtype=author&query=Takai%2C+S">S. Takai</a>, <a href="/search/?searchtype=author&query=Otsubo%2C+T">T. Otsubo</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Ochiai%2C+A">A. Ochiai</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="1509.09043v1-abstract-short" style="display: inline;"> Hexagonal-to-orthorhombic structural transitions in RAl$_3$C$_3$ have been studied by X-ray diffraction for R=Yb, Tm, Er, Dy, and Lu. We report how orthorhombic domains are controlled by adjusting external magnetic fields. It is shown that orthorhombic domains in RAl$_3$C$_3$ can be aligned by the field when the R ion is magnetic. It is also shown that a single-domain state can be switched to anot… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.09043v1-abstract-full').style.display = 'inline'; document.getElementById('1509.09043v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.09043v1-abstract-full" style="display: none;"> Hexagonal-to-orthorhombic structural transitions in RAl$_3$C$_3$ have been studied by X-ray diffraction for R=Yb, Tm, Er, Dy, and Lu. We report how orthorhombic domains are controlled by adjusting external magnetic fields. It is shown that orthorhombic domains in RAl$_3$C$_3$ can be aligned by the field when the R ion is magnetic. It is also shown that a single-domain state can be switched to another single-domain state by the field even in paramagnetic states with small induced moments. For R=Lu, however, it was not possible to change the multidomain state by a field of up to 70 kOe. We discuss that domain selection and switching are caused by magnetic anisotropies in the orthorhombic phase of RAl$_3$C$_3$. We also propose an idea to explain the field-induced antiferromagnetism revealed by Khalyavin et al. [Phys. Rev. B \textbf{87}, 220406 (2013)]. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.09043v1-abstract-full').style.display = 'none'; document.getElementById('1509.09043v1-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> 30 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">8 pages, 10 figures, 1 table, accepted in J. Phys. Soc. Jpn</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J. Phys. Soc. Jpn. 84, 114712 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1509.03724">arXiv:1509.03724</a> <span> [<a href="https://arxiv.org/pdf/1509.03724">pdf</a>, <a href="https://arxiv.org/ps/1509.03724">ps</a>, <a href="https://arxiv.org/format/1509.03724">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</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.nuclphysa.2015.11.011">10.1016/j.nuclphysa.2015.11.011 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for double-beta decay of 136Xe to excited states of 136Ba with the KamLAND-Zen experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Collaboration%2C+K">KamLAND-Zen Collaboration</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Asakura%2C+K">K. Asakura</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Ishikawa%2C+T">T. Ishikawa</a>, <a href="/search/?searchtype=author&query=Ishio%2C+S">S. Ishio</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Motoki%2C+D">D. Motoki</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Obara%2C+S">S. Obara</a>, <a href="/search/?searchtype=author&query=Otani%2C+M">M. Otani</a>, <a href="/search/?searchtype=author&query=Oura%2C+T">T. Oura</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/?searchtype=author&query=Shirahata%2C+Y">Y. Shirahata</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/?searchtype=author&query=Tachibana%2C+H">H. Tachibana</a> , et al. (21 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="1509.03724v2-abstract-short" style="display: inline;"> A search for double-beta decays of 136Xe to excited states of 136Ba has been performed with the first phase data set of the KamLAND-Zen experiment. The 0+1, 2+1 and 2+2 transitions of 0谓\{beta}\{beta} decay were evaluated in an exposure of 89.5kg-yr of 136Xe, while the same transitions of 2谓\{beta}\{beta} decay were evaluated in an exposure of 61.8kg-yr. No excess over background was found for all… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.03724v2-abstract-full').style.display = 'inline'; document.getElementById('1509.03724v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.03724v2-abstract-full" style="display: none;"> A search for double-beta decays of 136Xe to excited states of 136Ba has been performed with the first phase data set of the KamLAND-Zen experiment. The 0+1, 2+1 and 2+2 transitions of 0谓\{beta}\{beta} decay were evaluated in an exposure of 89.5kg-yr of 136Xe, while the same transitions of 2谓\{beta}\{beta} decay were evaluated in an exposure of 61.8kg-yr. No excess over background was found for all decay modes. The lower half-life limits of the 2+1 state transitions of 0谓\{beta}\{beta} and 2谓\{beta}\{beta} decay were improved to T(0谓, 0+ \rightarrow 2+) > 2.6\times10^25 yr and T(2谓, 0+ \rightarrow 2+) > 4.6\times10^23 yr (90% C.L.), respectively. We report on the first experimental lower half-life limits for the transitions to the 0+1 state of 136Xe for 0谓\{beta}\{beta} and 2谓\{beta}\{beta} decay. They are T (0谓, 0+ \rightarrow 0+) > 2.4\times10^25 yr and T(2谓, 0+ \rightarrow 0+) > 8.3\times10^23 yr (90% C.L.). The transitions to the 2+2 states are also evaluated for the first time to be T(0谓, 0+ \rightarrow 2+) > 2.6\times10^25 yr and T(2谓, 0+ \rightarrow 2+) > 9.0\times10^23 yr (90% C.L.). These results are compared to recent theoretical predictions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.03724v2-abstract-full').style.display = 'none'; document.getElementById('1509.03724v2-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 December, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">16 pages, 4 figures. Published in Nuclear Physics A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1506.01267">arXiv:1506.01267</a> <span> [<a href="https://arxiv.org/pdf/1506.01267">pdf</a>, <a href="https://arxiv.org/ps/1506.01267">ps</a>, <a href="https://arxiv.org/format/1506.01267">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</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/10.3847/0004-637X/822/2/65">10.3847/0004-637X/822/2/65 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurements of cosmic-ray proton and helium spectra from the BESS-Polar long-duration balloon flights over Antarctica </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Fuke%2C+H">H. Fuke</a>, <a href="/search/?searchtype=author&query=Haino%2C+S">S. Haino</a>, <a href="/search/?searchtype=author&query=Hams%2C+T">T. Hams</a>, <a href="/search/?searchtype=author&query=Hasegawa%2C+M">M. Hasegawa</a>, <a href="/search/?searchtype=author&query=Horikoshi%2C+A">A. Horikoshi</a>, <a href="/search/?searchtype=author&query=Itazaki%2C+A">A. Itazaki</a>, <a href="/search/?searchtype=author&query=Kim%2C+K+C">K. C. Kim</a>, <a href="/search/?searchtype=author&query=Kumazawa%2C+T">T. Kumazawa</a>, <a href="/search/?searchtype=author&query=Kusumoto%2C+A">A. Kusumoto</a>, <a href="/search/?searchtype=author&query=Lee%2C+M+H">M. H. Lee</a>, <a href="/search/?searchtype=author&query=Makida%2C+Y">Y. Makida</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Matsukawa%2C+Y">Y. Matsukawa</a>, <a href="/search/?searchtype=author&query=Matsumoto%2C+K">K. Matsumoto</a>, <a href="/search/?searchtype=author&query=Mitchell%2C+J+W">J. W. Mitchell</a>, <a href="/search/?searchtype=author&query=Myers%2C+Z">Z. Myers</a>, <a href="/search/?searchtype=author&query=Nishimura%2C+J">J. Nishimura</a>, <a href="/search/?searchtype=author&query=Nozaki%2C+M">M. Nozaki</a>, <a href="/search/?searchtype=author&query=Orito%2C+R">R. Orito</a>, <a href="/search/?searchtype=author&query=Ormes%2C+J+F">J. F. Ormes</a>, <a href="/search/?searchtype=author&query=Picot-Clemente%2C+N">N. Picot-Clemente</a>, <a href="/search/?searchtype=author&query=Sakai%2C+K">K. Sakai</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Seo%2C+E+S">E. S. Seo</a> , et al. (12 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="1506.01267v2-abstract-short" style="display: inline;"> The BESS-Polar Collaboration measured the energy spectra of cosmic-ray protons and helium during two long-duration balloon flights over Antarctica in December 2004 and December 2007, at substantially different levels of solar modulation. Proton and helium spectra probe the origin and propagation history of cosmic rays in the galaxy, and are essential to calculations of the expected spectra of cosm… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.01267v2-abstract-full').style.display = 'inline'; document.getElementById('1506.01267v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1506.01267v2-abstract-full" style="display: none;"> The BESS-Polar Collaboration measured the energy spectra of cosmic-ray protons and helium during two long-duration balloon flights over Antarctica in December 2004 and December 2007, at substantially different levels of solar modulation. Proton and helium spectra probe the origin and propagation history of cosmic rays in the galaxy, and are essential to calculations of the expected spectra of cosmic-ray antiprotons, positrons, and electrons from interactions of primary cosmic-ray nuclei with the interstellar gas, and to calculations of atmospheric muons and neutrinos. We report absolute spectra at the top of the atmosphere for cosmic-ray protons in the kinetic energy range 0.2-160 GeV and helium nuclei 0.15-80 GeV/nucleon. The corresponding magnetic rigidity ranges are 0.6-160 GV for protons and 1.1-160 GV for helium. These spectra are compared to measurements from previous BESS flights and from ATIC-2, PAMELA, and AMS-02. We also report the ratio of the proton and helium fluxes from 1.1 GV to 160 GV and compare to ratios from PAMELA and AMS-02. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.01267v2-abstract-full').style.display = 'none'; document.getElementById('1506.01267v2-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> 30 August, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 June, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">23 pages, 11 figures, Accepted for publication in The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1506.01175">arXiv:1506.01175</a> <span> [<a href="https://arxiv.org/pdf/1506.01175">pdf</a>, <a href="https://arxiv.org/ps/1506.01175">ps</a>, <a href="https://arxiv.org/format/1506.01175">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</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/10.3847/0004-637X/818/1/91">10.3847/0004-637X/818/1/91 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> KamLAND Sensitivity to Neutrinos from Pre-Supernova Stars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Asakura%2C+K">K. Asakura</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Ishikawa%2C+T">T. Ishikawa</a>, <a href="/search/?searchtype=author&query=Ishio%2C+S">S. Ishio</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Motoki%2C+D">D. Motoki</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Obara%2C+S">S. Obara</a>, <a href="/search/?searchtype=author&query=Oura%2C+T">T. Oura</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/?searchtype=author&query=Shirahata%2C+Y">Y. Shirahata</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/?searchtype=author&query=Tachibana%2C+H">H. Tachibana</a>, <a href="/search/?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a>, <a href="/search/?searchtype=author&query=Watanabe%2C+H">H. Watanabe</a> , et al. (22 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="1506.01175v4-abstract-short" style="display: inline;"> In the late stages of nuclear burning for massive stars ($M>8~M_{\sun}$), the production of neutrino-antineutrino pairs through various processes becomes the dominant stellar cooling mechanism. As the star evolves, the energy of these neutrinos increases and in the days preceding the supernova a significant fraction of emitted electron anti-neutrinos exceeds the energy threshold for inverse beta d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.01175v4-abstract-full').style.display = 'inline'; document.getElementById('1506.01175v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1506.01175v4-abstract-full" style="display: none;"> In the late stages of nuclear burning for massive stars ($M>8~M_{\sun}$), the production of neutrino-antineutrino pairs through various processes becomes the dominant stellar cooling mechanism. As the star evolves, the energy of these neutrinos increases and in the days preceding the supernova a significant fraction of emitted electron anti-neutrinos exceeds the energy threshold for inverse beta decay on free hydrogen. This is the golden channel for liquid scintillator detectors because the coincidence signature allows for significant reductions in background signals. We find that the kiloton-scale liquid scintillator detector KamLAND can detect these pre-supernova neutrinos from a star with a mass of $25~M_{\sun}$ at a distance less than 690~pc with 3$蟽$ significance before the supernova. This limit is dependent on the neutrino mass ordering and background levels. KamLAND takes data continuously and can provide a supernova alert to the community. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1506.01175v4-abstract-full').style.display = 'none'; document.getElementById('1506.01175v4-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 January, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 June, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">19 pages, 6 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1503.02137">arXiv:1503.02137</a> <span> [<a href="https://arxiv.org/pdf/1503.02137">pdf</a>, <a href="https://arxiv.org/ps/1503.02137">ps</a>, <a href="https://arxiv.org/format/1503.02137">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="High Energy Physics - Experiment">hep-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/10.1088/0004-637X/806/1/87">10.1088/0004-637X/806/1/87 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Study of electron anti-neutrinos associated with gamma-ray bursts using KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Asakura%2C+K">K. Asakura</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Hachiya%2C+T">T. Hachiya</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Ishikawa%2C+T">T. Ishikawa</a>, <a href="/search/?searchtype=author&query=Ishio%2C+S">S. Ishio</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Motoki%2C+D">D. Motoki</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Obara%2C+S">S. Obara</a>, <a href="/search/?searchtype=author&query=Oki%2C+Y">Y. Oki</a>, <a href="/search/?searchtype=author&query=Oura%2C+T">T. Oura</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/?searchtype=author&query=Shirahata%2C+Y">Y. Shirahata</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/?searchtype=author&query=Tachibana%2C+H">H. Tachibana</a>, <a href="/search/?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a> , et al. (23 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="1503.02137v2-abstract-short" style="display: inline;"> We search for electron anti-neutrinos ($\overline谓_e$) from long and short-duration gamma-ray bursts~(GRBs) using data taken by the KamLAND detector from August 2002 to June 2013. No statistically significant excess over the background level is found. We place the tightest upper limits on $\overline谓_e$ fluence from GRBs below 7 MeV and place first constraints on the relation between… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.02137v2-abstract-full').style.display = 'inline'; document.getElementById('1503.02137v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.02137v2-abstract-full" style="display: none;"> We search for electron anti-neutrinos ($\overline谓_e$) from long and short-duration gamma-ray bursts~(GRBs) using data taken by the KamLAND detector from August 2002 to June 2013. No statistically significant excess over the background level is found. We place the tightest upper limits on $\overline谓_e$ fluence from GRBs below 7 MeV and place first constraints on the relation between $\overline谓_e$ luminosity and effective temperature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.02137v2-abstract-full').style.display = 'none'; document.getElementById('1503.02137v2-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> 15 June, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 March, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">16 pages and 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 806 87 2015 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1405.6190">arXiv:1405.6190</a> <span> [<a href="https://arxiv.org/pdf/1405.6190">pdf</a>, <a href="https://arxiv.org/ps/1405.6190">ps</a>, <a href="https://arxiv.org/format/1405.6190">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-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 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.92.055808">10.1103/PhysRevC.92.055808 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> 7Be Solar Neutrino Measurement with KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Hanakago%2C+H">H. Hanakago</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Ishikawa%2C+H">H. Ishikawa</a>, <a href="/search/?searchtype=author&query=Kishimoto%2C+Y">Y. Kishimoto</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+R">R. Matsuda</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Motoki%2C+D">D. Motoki</a>, <a href="/search/?searchtype=author&query=Nakajima%2C+K">K. Nakajima</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Obata%2C+A">A. Obata</a>, <a href="/search/?searchtype=author&query=Oki%2C+A">A. Oki</a>, <a href="/search/?searchtype=author&query=Oki%2C+Y">Y. Oki</a>, <a href="/search/?searchtype=author&query=Otani%2C+M">M. Otani</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a>, <a href="/search/?searchtype=author&query=Watanabe%2C+H">H. Watanabe</a> , et al. (46 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="1405.6190v2-abstract-short" style="display: inline;"> We report a measurement of the neutrino-electron elastic scattering rate of 862 keV 7Be solar neutrinos based on a 165.4 kton-day exposure of KamLAND. The observed rate is 582 +/- 90 (kton-day)^-1, which corresponds to a 862 keV 7Be solar neutrino flux of (3.26 +/- 0.50) x 10^9 cm^-2s^-1, assuming a pure electron flavor flux. Comparing this flux with the standard solar model prediction and further… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.6190v2-abstract-full').style.display = 'inline'; document.getElementById('1405.6190v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1405.6190v2-abstract-full" style="display: none;"> We report a measurement of the neutrino-electron elastic scattering rate of 862 keV 7Be solar neutrinos based on a 165.4 kton-day exposure of KamLAND. The observed rate is 582 +/- 90 (kton-day)^-1, which corresponds to a 862 keV 7Be solar neutrino flux of (3.26 +/- 0.50) x 10^9 cm^-2s^-1, assuming a pure electron flavor flux. Comparing this flux with the standard solar model prediction and further assuming three flavor mixing, a nu_e survival probability of 0.66 +/- 0.14 is determined from the KamLAND data. Utilizing a global three flavor oscillation analysis, we obtain a total 7Be solar neutrino flux of (5.82 +/- 0.98) x 10^9 cm^-2s^-1, which is consistent with the standard solar model predictions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1405.6190v2-abstract-full').style.display = 'none'; document.getElementById('1405.6190v2-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> 30 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 May, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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, 6 figures, submitted to 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/1312.0896">arXiv:1312.0896</a> <span> [<a href="https://arxiv.org/pdf/1312.0896">pdf</a>, <a href="https://arxiv.org/format/1312.0896">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> CeLAND: search for a 4th light neutrino state with a 3 PBq 144Ce-144Pr electron antineutrino generator in KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Ishikawa%2C+H">H. Ishikawa</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+R">R. Matsuda</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Motoki%2C+D">D. Motoki</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Oki%2C+Y">Y. Oki</a>, <a href="/search/?searchtype=author&query=Otani%2C+M">M. Otani</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Suekane%2C+F">F. Suekane</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/?searchtype=author&query=Takemoto%2C+Y">Y. Takemoto</a>, <a href="/search/?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a>, <a href="/search/?searchtype=author&query=Watanabe%2C+H">H. Watanabe</a>, <a href="/search/?searchtype=author&query=Xu%2C+B+D">B. D. Xu</a>, <a href="/search/?searchtype=author&query=Yamada%2C+S">S. Yamada</a> , et al. (41 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="1312.0896v2-abstract-short" style="display: inline;"> The reactor neutrino and gallium anomalies can be tested with a 3-4 PBq (75-100 kCi scale) 144Ce-144Pr antineutrino beta-source deployed at the center or next to a large low-background liquid scintillator detector. The antineutrino generator will be produced by the Russian reprocessing plant PA Mayak as early as 2014, transported to Japan, and deployed in the Kamioka Liquid Scintillator Anti-Neutr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.0896v2-abstract-full').style.display = 'inline'; document.getElementById('1312.0896v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1312.0896v2-abstract-full" style="display: none;"> The reactor neutrino and gallium anomalies can be tested with a 3-4 PBq (75-100 kCi scale) 144Ce-144Pr antineutrino beta-source deployed at the center or next to a large low-background liquid scintillator detector. The antineutrino generator will be produced by the Russian reprocessing plant PA Mayak as early as 2014, transported to Japan, and deployed in the Kamioka Liquid Scintillator Anti-Neutrino Detector (KamLAND) as early as 2015. KamLAND's 13 m diameter target volume provides a suitable environment to measure the energy and position dependence of the detected neutrino flux. A characteristic oscillation pattern would be visible for a baseline of about 10 m or less, providing a very clean signal of neutrino disappearance into a yet-unknown, sterile neutrino state. This will provide a comprehensive test of the electron dissaperance neutrino anomalies and could lead to the discovery of a 4th neutrino state for Delta_m^2 > 0.1 eV^2 and sin^2(2theta) > 0.05. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1312.0896v2-abstract-full').style.display = 'none'; document.getElementById('1312.0896v2-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 April, 2014; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">67 pages, 50 figures. Th. Lasserre thanks the European Research Council for support under the Starting Grant StG-307184</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1309.6805">arXiv:1309.6805</a> <span> [<a href="https://arxiv.org/pdf/1309.6805">pdf</a>, <a href="https://arxiv.org/format/1309.6805">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> White paper: CeLAND - Investigation of the reactor antineutrino anomaly with an intense 144Ce-144Pr antineutrino source in KamLAND </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Hayashida%2C+S">S. Hayashida</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Ishidoshiro%2C+K">K. Ishidoshiro</a>, <a href="/search/?searchtype=author&query=Ishikawa%2C+H">H. Ishikawa</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+R">R. Matsuda</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Motoki%2C+D">D. Motoki</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Oki%2C+Y">Y. Oki</a>, <a href="/search/?searchtype=author&query=Otani%2C+M">M. Otani</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Suekane%2C+F">F. Suekane</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/?searchtype=author&query=Takemoto%2C+Y">Y. Takemoto</a>, <a href="/search/?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a>, <a href="/search/?searchtype=author&query=Watanabe%2C+H">H. Watanabe</a>, <a href="/search/?searchtype=author&query=Xu%2C+B+D">B. D. Xu</a>, <a href="/search/?searchtype=author&query=Yamada%2C+S">S. Yamada</a> , et al. (35 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="1309.6805v2-abstract-short" style="display: inline;"> We propose to test for short baseline neutrino oscillations, implied by the recent reevaluation of the reactor antineutrino flux and by anomalous results from the gallium solar neutrino detectors. The test will consist of producing a 75 kCi 144Ce - 144Pr antineutrino source to be deployed in the Kamioka Liquid Scintillator Anti-Neutrino Detector (KamLAND). KamLAND's 13m diameter target volume prov… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1309.6805v2-abstract-full').style.display = 'inline'; document.getElementById('1309.6805v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1309.6805v2-abstract-full" style="display: none;"> We propose to test for short baseline neutrino oscillations, implied by the recent reevaluation of the reactor antineutrino flux and by anomalous results from the gallium solar neutrino detectors. The test will consist of producing a 75 kCi 144Ce - 144Pr antineutrino source to be deployed in the Kamioka Liquid Scintillator Anti-Neutrino Detector (KamLAND). KamLAND's 13m diameter target volume provides a suitable environment to measure energy and position dependence of the detected neutrino flux. A characteristic oscillation pattern would be visible for a baseline of about 10 m or less, providing a very clean signal of neutrino disappearance into a yet-unknown, "sterile" state. Such a measurement will be free of any reactor-related uncertainties. After 1.5 years of data taking the Reactor Antineutrino Anomaly parameter space will be tested at > 95% C.L. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1309.6805v2-abstract-full').style.display = 'none'; document.getElementById('1309.6805v2-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 October, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 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">White paper prepared for Snowmass-2013; slightly different author list</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1307.3494">arXiv:1307.3494</a> <span> [<a href="https://arxiv.org/pdf/1307.3494">pdf</a>, <a href="https://arxiv.org/ps/1307.3494">ps</a>, <a href="https://arxiv.org/format/1307.3494">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Strongly Correlated Electrons">cond-mat.str-el</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/10.3938/jkps.62.2088">10.3938/jkps.62.2088 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Singlet-triplet Crossover in the Two-dimensional Dimer Spin System YbAl3C3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kittaka%2C+S">Shunichiro Kittaka</a>, <a href="/search/?searchtype=author&query=Sugiyama%2C+T">Tomoyoshi Sugiyama</a>, <a href="/search/?searchtype=author&query=Shimura%2C+Y">Yasuyuki Shimura</a>, <a href="/search/?searchtype=author&query=Sakakibara%2C+T">Toshiro Sakakibara</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">Saori Matsuda</a>, <a href="/search/?searchtype=author&query=Ochiai%2C+A">Akira Ochiai</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="1307.3494v1-abstract-short" style="display: inline;"> Low-temperature magnetization (M) measurements down to 0.1 K have been performed in magnetic fields up to 14.5 T for a single piece of a tiny single-crystalline sample (0.2 mg weight) of the spin-gap system YbAl3C3. At the base temperature of 0.1 K, several metamagnetic transitions were clearly observed for H // c in the range 6 T < H < 9 T whereas only two transitions were observed, one at 4.8 T… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.3494v1-abstract-full').style.display = 'inline'; document.getElementById('1307.3494v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1307.3494v1-abstract-full" style="display: none;"> Low-temperature magnetization (M) measurements down to 0.1 K have been performed in magnetic fields up to 14.5 T for a single piece of a tiny single-crystalline sample (0.2 mg weight) of the spin-gap system YbAl3C3. At the base temperature of 0.1 K, several metamagnetic transitions were clearly observed for H // c in the range 6 T < H < 9 T whereas only two transitions were observed, one at 4.8 T and the other at 6.6 T, for H // a. At fields above 9 T, the magnetization becomes almost saturated for both H // a and H // c. The present results indicate that a singlet-triplet crossover occurs in a relatively narrow field range, suggesting a rather weak interdimer interaction in spite of the nearly triangular lattice of Yb ions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.3494v1-abstract-full').style.display = 'none'; document.getElementById('1307.3494v1-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 July, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">5 pages, 6 figures, proceedings of ICM 2012</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J. Korean Phys. Soc. 62, 2088 (2013) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1205.6372">arXiv:1205.6372</a> <span> [<a href="https://arxiv.org/pdf/1205.6372">pdf</a>, <a href="https://arxiv.org/ps/1205.6372">ps</a>, <a href="https://arxiv.org/format/1205.6372">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</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.86.021601">10.1103/PhysRevC.86.021601 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Limits on Majoron-emitting double-beta decays of Xe-136 in the KamLAND-Zen experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Collaboration%2C+K">KamLAND-Zen Collaboration</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Gando%2C+A">A. Gando</a>, <a href="/search/?searchtype=author&query=Gando%2C+Y">Y. Gando</a>, <a href="/search/?searchtype=author&query=Hanakago%2C+H">H. Hanakago</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+H">H. Ikeda</a>, <a href="/search/?searchtype=author&query=Inoue%2C+K">K. Inoue</a>, <a href="/search/?searchtype=author&query=Kato%2C+R">R. Kato</a>, <a href="/search/?searchtype=author&query=Koga%2C+M">M. Koga</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Nakada%2C+T">T. Nakada</a>, <a href="/search/?searchtype=author&query=Nakamura%2C+K">K. Nakamura</a>, <a href="/search/?searchtype=author&query=Obata%2C+A">A. Obata</a>, <a href="/search/?searchtype=author&query=Oki%2C+A">A. Oki</a>, <a href="/search/?searchtype=author&query=Ono%2C+Y">Y. Ono</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+I">I. Shimizu</a>, <a href="/search/?searchtype=author&query=Shirai%2C+J">J. Shirai</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+A">A. Suzuki</a>, <a href="/search/?searchtype=author&query=Takemoto%2C+Y">Y. Takemoto</a>, <a href="/search/?searchtype=author&query=Tamae%2C+K">K. Tamae</a>, <a href="/search/?searchtype=author&query=Ueshima%2C+K">K. Ueshima</a>, <a href="/search/?searchtype=author&query=Watanabe%2C+H">H. Watanabe</a>, <a href="/search/?searchtype=author&query=Xu%2C+B+D">B. D. Xu</a>, <a href="/search/?searchtype=author&query=Yamada%2C+S">S. Yamada</a> , et al. (16 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="1205.6372v2-abstract-short" style="display: inline;"> We present limits on Majoron-emitting neutrinoless double-beta decay modes based on an exposure of 112.3 days with 125 kg of Xe-136. In particular, a lower limit on the ordinary (spectral index n = 1) Majoron-emitting decay half-life of Xe-136 is obtained as T_{1/2}^{0谓蠂^{0}} > 2.6 x 10^{24} yr at 90% C.L., a factor of five more stringent than previous limits. The corresponding upper limit on the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1205.6372v2-abstract-full').style.display = 'inline'; document.getElementById('1205.6372v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1205.6372v2-abstract-full" style="display: none;"> We present limits on Majoron-emitting neutrinoless double-beta decay modes based on an exposure of 112.3 days with 125 kg of Xe-136. In particular, a lower limit on the ordinary (spectral index n = 1) Majoron-emitting decay half-life of Xe-136 is obtained as T_{1/2}^{0谓蠂^{0}} > 2.6 x 10^{24} yr at 90% C.L., a factor of five more stringent than previous limits. The corresponding upper limit on the effective Majoron-neutrino coupling, using a range of available nuclear matrix calculations, is <g_{ee}> < (0.8 - 1.6) x 10^{-5}. This excludes a previously unconstrained region of parameter space and strongly limits the possible contribution of ordinary Majoron emission modes to 0谓尾尾decay for neutrino masses in the inverted hierarchy scheme. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1205.6372v2-abstract-full').style.display = 'none'; document.getElementById('1205.6372v2-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> 7 August, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 May, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">4 pages, 3 figures (1 figure added). Published version in PRC rapid communication</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.C86:021601,2012 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1201.2967">arXiv:1201.2967</a> <span> [<a href="https://arxiv.org/pdf/1201.2967">pdf</a>, <a href="https://arxiv.org/ps/1201.2967">ps</a>, <a href="https://arxiv.org/format/1201.2967">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/PhysRevLett.108.131301">10.1103/PhysRevLett.108.131301 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Antihelium with the BESS-Polar Spectrometer </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Fuke%2C+H">H. Fuke</a>, <a href="/search/?searchtype=author&query=Haino%2C+S">S. Haino</a>, <a href="/search/?searchtype=author&query=Hams%2C+T">T. Hams</a>, <a href="/search/?searchtype=author&query=Hasegawa%2C+M">M. Hasegawa</a>, <a href="/search/?searchtype=author&query=Horikoshi%2C+A">A. Horikoshi</a>, <a href="/search/?searchtype=author&query=Itazaki%2C+A">A. Itazaki</a>, <a href="/search/?searchtype=author&query=Kim%2C+K+C">K. C. Kim</a>, <a href="/search/?searchtype=author&query=Kumazawa%2C+T">T. Kumazawa</a>, <a href="/search/?searchtype=author&query=Kusumoto%2C+A">A. Kusumoto</a>, <a href="/search/?searchtype=author&query=Lee%2C+M+H">M. H. Lee</a>, <a href="/search/?searchtype=author&query=Makida%2C+Y">Y. Makida</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Matsukawa%2C+Y">Y. Matsukawa</a>, <a href="/search/?searchtype=author&query=Matsumoto%2C+K">K. Matsumoto</a>, <a href="/search/?searchtype=author&query=Mitchell%2C+J+W">J. W. Mitchell</a>, <a href="/search/?searchtype=author&query=Myers%2C+Z">Z. Myers</a>, <a href="/search/?searchtype=author&query=Nishimura%2C+J">J. Nishimura</a>, <a href="/search/?searchtype=author&query=Nozaki%2C+M">M. Nozaki</a>, <a href="/search/?searchtype=author&query=Orito%2C+R">R. Orito</a>, <a href="/search/?searchtype=author&query=Ormes%2C+J+F">J. F. Ormes</a>, <a href="/search/?searchtype=author&query=Sakai%2C+K">K. Sakai</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Seo%2C+E+S">E. S. Seo</a>, <a href="/search/?searchtype=author&query=Shikaze%2C+Y">Y. Shikaze</a> , et al. (11 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="1201.2967v1-abstract-short" style="display: inline;"> In two long-duration balloon flights over Antarctica, the BESS-Polar collaboration has searched for antihelium in the cosmic radiation with higher sensitivity than any reported investigation. BESS- Polar I flew in 2004, observing for 8.5 days. BESS-Polar II flew in 2007-2008, observing for 24.5 days. No antihelium candidate was found in BESS-Polar I data among 8.4\times 10^6 |Z| = 2 nuclei from 1.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.2967v1-abstract-full').style.display = 'inline'; document.getElementById('1201.2967v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1201.2967v1-abstract-full" style="display: none;"> In two long-duration balloon flights over Antarctica, the BESS-Polar collaboration has searched for antihelium in the cosmic radiation with higher sensitivity than any reported investigation. BESS- Polar I flew in 2004, observing for 8.5 days. BESS-Polar II flew in 2007-2008, observing for 24.5 days. No antihelium candidate was found in BESS-Polar I data among 8.4\times 10^6 |Z| = 2 nuclei from 1.0 to 20 GV or in BESS-Polar II data among 4.0\times 10^7 |Z| = 2 nuclei from 1.0 to 14 GV. Assuming antihelium to have the same spectral shape as helium, a 95% confidence upper limit of 6.9 \times 10^-8 was determined by combining all the BESS data, including the two BESS-Polar flights. With no assumed antihelium spectrum and a weighted average of the lowest antihelium efficiencies from 1.6 to 14 GV, an upper limit of 1.0 \times 10^-7 was determined for the combined BESS-Polar data. These are the most stringent limits obtained to date. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.2967v1-abstract-full').style.display = 'none'; document.getElementById('1201.2967v1-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 January, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">4 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/1107.6000">arXiv:1107.6000</a> <span> [<a href="https://arxiv.org/pdf/1107.6000">pdf</a>, <a href="https://arxiv.org/ps/1107.6000">ps</a>, <a href="https://arxiv.org/format/1107.6000">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</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.108.051102">10.1103/PhysRevLett.108.051102 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the cosmic-ray antiproton spectrum at solar minimum with a long-duration balloon flight over Antarctica </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Fuke%2C+H">H. Fuke</a>, <a href="/search/?searchtype=author&query=Haino%2C+S">S. Haino</a>, <a href="/search/?searchtype=author&query=Hams%2C+T">T. Hams</a>, <a href="/search/?searchtype=author&query=Hasegawa%2C+M">M. Hasegawa</a>, <a href="/search/?searchtype=author&query=Horikoshi%2C+A">A. Horikoshi</a>, <a href="/search/?searchtype=author&query=Kim%2C+K+C">K. C. Kim</a>, <a href="/search/?searchtype=author&query=Kusumoto%2C+A">A. Kusumoto</a>, <a href="/search/?searchtype=author&query=Lee%2C+M+H">M. H. Lee</a>, <a href="/search/?searchtype=author&query=Makida%2C+Y">Y. Makida</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Matsukawa%2C+Y">Y. Matsukawa</a>, <a href="/search/?searchtype=author&query=Mitchell%2C+J+W">J. W. Mitchell</a>, <a href="/search/?searchtype=author&query=Nishimura%2C+J">J. Nishimura</a>, <a href="/search/?searchtype=author&query=Nozaki%2C+M">M. Nozaki</a>, <a href="/search/?searchtype=author&query=Orito%2C+R">R. Orito</a>, <a href="/search/?searchtype=author&query=Ormes%2C+J+F">J. F. Ormes</a>, <a href="/search/?searchtype=author&query=Sakai%2C+K">K. Sakai</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Seo%2C+E+S">E. S. Seo</a>, <a href="/search/?searchtype=author&query=Shinoda%2C+R">R. Shinoda</a>, <a href="/search/?searchtype=author&query=Streitmatter%2C+R+E">R. E. Streitmatter</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+J">J. Suzuki</a>, <a href="/search/?searchtype=author&query=Tanaka%2C+K">K. Tanaka</a>, <a href="/search/?searchtype=author&query=Thakur%2C+N">N. Thakur</a> , et al. (4 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="1107.6000v2-abstract-short" style="display: inline;"> The energy spectrum of cosmic-ray antiprotons from 0.17 to 3.5 GeV has been measured using 7886 antiprotons detected by BESS-Polar II during a long-duration flight over Antarctica near solar minimum in December 2007 and January 2008. This shows good consistency with secondary antiproton calculations. Cosmologically primary antiprotons have been investigated by comparing measured and calculated ant… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1107.6000v2-abstract-full').style.display = 'inline'; document.getElementById('1107.6000v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1107.6000v2-abstract-full" style="display: none;"> The energy spectrum of cosmic-ray antiprotons from 0.17 to 3.5 GeV has been measured using 7886 antiprotons detected by BESS-Polar II during a long-duration flight over Antarctica near solar minimum in December 2007 and January 2008. This shows good consistency with secondary antiproton calculations. Cosmologically primary antiprotons have been investigated by comparing measured and calculated antiproton spectra. BESS-Polar II data show no evidence of primary antiprotons from evaporation of primordial black holes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1107.6000v2-abstract-full').style.display = 'none'; document.getElementById('1107.6000v2-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> 10 December, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 July, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">4 pages, 4 figures, submitted to Physical Review Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/0805.1754">arXiv:0805.1754</a> <span> [<a href="https://arxiv.org/pdf/0805.1754">pdf</a>, <a href="https://arxiv.org/ps/0805.1754">ps</a>, <a href="https://arxiv.org/format/0805.1754">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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.2008.10.053">10.1016/j.physletb.2008.10.053 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of cosmic-ray low-energy antiproton spectrum with the first BESS-Polar Antarctic flight </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Fuke%2C+H">H. Fuke</a>, <a href="/search/?searchtype=author&query=Haino%2C+S">S. Haino</a>, <a href="/search/?searchtype=author&query=Hams%2C+T">T. Hams</a>, <a href="/search/?searchtype=author&query=Itazaki%2C+A">A. Itazaki</a>, <a href="/search/?searchtype=author&query=Kim%2C+K+C">K. C. Kim</a>, <a href="/search/?searchtype=author&query=Kumazawa%2C+T">T. Kumazawa</a>, <a href="/search/?searchtype=author&query=Lee%2C+M+H">M. H. Lee</a>, <a href="/search/?searchtype=author&query=Makida%2C+Y">Y. Makida</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Matsumoto%2C+K">K. Matsumoto</a>, <a href="/search/?searchtype=author&query=Mitchell%2C+J+W">J. W. Mitchell</a>, <a href="/search/?searchtype=author&query=Moiseev%2C+A+A">A. A. Moiseev</a>, <a href="/search/?searchtype=author&query=Myers%2C+Z">Z. Myers</a>, <a href="/search/?searchtype=author&query=Nishimura%2C+J">J. Nishimura</a>, <a href="/search/?searchtype=author&query=Nozaki%2C+M">M. Nozaki</a>, <a href="/search/?searchtype=author&query=Orito%2C+R">R. Orito</a>, <a href="/search/?searchtype=author&query=Ormes%2C+J+F">J. F. Ormes</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Seo%2C+E+S">E. S. Seo</a>, <a href="/search/?searchtype=author&query=Shikaze%2C+Y">Y. Shikaze</a>, <a href="/search/?searchtype=author&query=Streitmatter%2C+R+E">R. E. Streitmatter</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+J">J. Suzuki</a>, <a href="/search/?searchtype=author&query=Takasugi%2C+Y">Y. Takasugi</a>, <a href="/search/?searchtype=author&query=Takeuchi%2C+K">K. Takeuchi</a> , et al. (5 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="0805.1754v2-abstract-short" style="display: inline;"> The BESS-Polar spectrometer had its first successful balloon flight over Antarctica in December 2004. During the 8.5-day long-duration flight, almost 0.9 billion events were recorded and 1,520 antiprotons were detected in the energy range 0.1-4.2 GeV. In this paper, we report the antiproton spectrum obtained, discuss the origin of cosmic-ray antiprotons, and use antiprotons to probe the effect o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0805.1754v2-abstract-full').style.display = 'inline'; document.getElementById('0805.1754v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="0805.1754v2-abstract-full" style="display: none;"> The BESS-Polar spectrometer had its first successful balloon flight over Antarctica in December 2004. During the 8.5-day long-duration flight, almost 0.9 billion events were recorded and 1,520 antiprotons were detected in the energy range 0.1-4.2 GeV. In this paper, we report the antiproton spectrum obtained, discuss the origin of cosmic-ray antiprotons, and use antiprotons to probe the effect of charge sign dependent drift in the solar modulation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('0805.1754v2-abstract-full').style.display = 'none'; document.getElementById('0805.1754v2-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> 21 September, 2008; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 May, 2008; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2008. </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">18 pages, 1 table, 5 figures, submitted to Physics Letters B</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Lett.B670:103-108,2008 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0611388">arXiv:astro-ph/0611388</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0611388">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0611388">ps</a>, <a href="https://arxiv.org/format/astro-ph/0611388">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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.astropartphys.2007.05.001">10.1016/j.astropartphys.2007.05.001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurements of 0.2 to 20 GeV/n cosmic-ray proton and helium spectra from 1997 through 2002 with the BESS spectrometer </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Shikaze%2C+Y">Y. Shikaze</a>, <a href="/search/?searchtype=author&query=Haino%2C+S">S. Haino</a>, <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Fuke%2C+H">H. Fuke</a>, <a href="/search/?searchtype=author&query=Hams%2C+T">T. Hams</a>, <a href="/search/?searchtype=author&query=Kim%2C+K+C">K. C. Kim</a>, <a href="/search/?searchtype=author&query=Makida%2C+Y">Y. Makida</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Mitchell%2C+J+W">J. W. Mitchell</a>, <a href="/search/?searchtype=author&query=Moiseev%2C+A+A">A. A. Moiseev</a>, <a href="/search/?searchtype=author&query=Nishimura%2C+J">J. Nishimura</a>, <a href="/search/?searchtype=author&query=Nozaki%2C+M">M. Nozaki</a>, <a href="/search/?searchtype=author&query=Orito%2C+S">S. Orito</a>, <a href="/search/?searchtype=author&query=Ormes%2C+J+F">J. F. Ormes</a>, <a href="/search/?searchtype=author&query=Sanuki%2C+T">T. Sanuki</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Seo%2C+E+S">E. S. Seo</a>, <a href="/search/?searchtype=author&query=Streitmatter%2C+R+E">R. E. Streitmatter</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+J">J. Suzuki</a>, <a href="/search/?searchtype=author&query=Tanaka%2C+K">K. Tanaka</a>, <a href="/search/?searchtype=author&query=Yamagami%2C+T">T. Yamagami</a>, <a href="/search/?searchtype=author&query=Yamamoto%2C+A">A. Yamamoto</a>, <a href="/search/?searchtype=author&query=Yoshida%2C+T">T. Yoshida</a>, <a href="/search/?searchtype=author&query=Yoshimura%2C+K">K. Yoshimura</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="astro-ph/0611388v3-abstract-short" style="display: inline;"> We measured low energy cosmic-ray proton and helium spectra in the kinetic energy range 0.215 - 21.5 GeV/n at different solar activities during a period from 1997 to 2002. The observations were carried out with the BESS spectrometer launched on a balloon at Lynn Lake, Canada. A calculation for the correction of secondary particle backgrounds from the overlying atmosphere was improved by using th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0611388v3-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0611388v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0611388v3-abstract-full" style="display: none;"> We measured low energy cosmic-ray proton and helium spectra in the kinetic energy range 0.215 - 21.5 GeV/n at different solar activities during a period from 1997 to 2002. The observations were carried out with the BESS spectrometer launched on a balloon at Lynn Lake, Canada. A calculation for the correction of secondary particle backgrounds from the overlying atmosphere was improved by using the measured spectra at small atmospheric depths ranging from 5 through 37 g/cm^2. The uncertainties including statistical and systematic errors of the obtained spectra at the top of atmosphere are 5-7 % for protons and 6-9 % for helium nuclei in the energy range 0.5 - 5 GeV/n. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0611388v3-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0611388v3-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> 21 April, 2007; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 November, 2006; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2006. </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">27 pages, 7 Tables, 9 figures, Submitted to Astroparticle Physics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astropart.Phys.28:154-167,2007 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0509577">arXiv:astro-ph/0509577</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0509577">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0509577">ps</a>, <a href="https://arxiv.org/format/astro-ph/0509577">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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.2005.11.042">10.1016/j.physletb.2005.11.042 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurements of Atmospheric Antiprotons </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Yamato%2C+K">K. Yamato</a>, <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Fuke%2C+H">H. Fuke</a>, <a href="/search/?searchtype=author&query=Haino%2C+S">S. Haino</a>, <a href="/search/?searchtype=author&query=Makida%2C+Y">Y. Makida</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Matsumoto%2C+H">H. Matsumoto</a>, <a href="/search/?searchtype=author&query=Mitchell%2C+J+W">J. W. Mitchell</a>, <a href="/search/?searchtype=author&query=Moiseev%2C+A+A">A. A. Moiseev</a>, <a href="/search/?searchtype=author&query=Nishimura%2C+J">J. Nishimura</a>, <a href="/search/?searchtype=author&query=Nozaki%2C+M">M. Nozaki</a>, <a href="/search/?searchtype=author&query=Orito%2C+S">S. Orito</a>, <a href="/search/?searchtype=author&query=Ormes%2C+J+F">J. F. Ormes</a>, <a href="/search/?searchtype=author&query=Sanuki%2C+T">T. Sanuki</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Seo%2C+E+S">E. S. Seo</a>, <a href="/search/?searchtype=author&query=Shikaze%2C+Y">Y. Shikaze</a>, <a href="/search/?searchtype=author&query=Streitmatter%2C+R+E">R. E. Streitmatter</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+J">J. Suzuki</a>, <a href="/search/?searchtype=author&query=Tanaka%2C+K">K. Tanaka</a>, <a href="/search/?searchtype=author&query=Yamagami%2C+T">T. Yamagami</a>, <a href="/search/?searchtype=author&query=Yamamoto%2C+A">A. Yamamoto</a>, <a href="/search/?searchtype=author&query=Yoshida%2C+T">T. Yoshida</a>, <a href="/search/?searchtype=author&query=Yoshimura%2C+K">K. Yoshimura</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="astro-ph/0509577v2-abstract-short" style="display: inline;"> We measured atmospheric antiproton spectra in the energy range 0.2 to 3.4 GeV, at sea level and at balloon altitude in the atmospheric depth range 4.5 to 26 g/cm^2. The observed energy spectra, including our previous measurements at mountain altitude, were compared with estimated spectra calculated on various assumptions regarding the energy distribution of antiprotons that interacted with air n… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0509577v2-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0509577v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0509577v2-abstract-full" style="display: none;"> We measured atmospheric antiproton spectra in the energy range 0.2 to 3.4 GeV, at sea level and at balloon altitude in the atmospheric depth range 4.5 to 26 g/cm^2. The observed energy spectra, including our previous measurements at mountain altitude, were compared with estimated spectra calculated on various assumptions regarding the energy distribution of antiprotons that interacted with air nuclei. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0509577v2-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0509577v2-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> 17 November, 2005; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 September, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2005. </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 PLB</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Lett.B632:475-479,2006 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0504361">arXiv:astro-ph/0504361</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0504361">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0504361">ps</a>, <a href="https://arxiv.org/format/astro-ph/0504361">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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.95.081101">10.1103/PhysRevLett.95.081101 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Cosmic-Ray Antideuterons </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fuke%2C+H">H. Fuke</a>, <a href="/search/?searchtype=author&query=Maeno%2C+T">T. Maeno</a>, <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Haino%2C+S">S. Haino</a>, <a href="/search/?searchtype=author&query=Makida%2C+Y">Y. Makida</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Matsumoto%2C+H">H. Matsumoto</a>, <a href="/search/?searchtype=author&query=Mitchell%2C+J+W">J. W. Mitchell</a>, <a href="/search/?searchtype=author&query=Moiseev%2C+A+A">A. A. Moiseev</a>, <a href="/search/?searchtype=author&query=Nishimura%2C+J">J. Nishimura</a>, <a href="/search/?searchtype=author&query=Nozaki%2C+M">M. Nozaki</a>, <a href="/search/?searchtype=author&query=Orito%2C+S">S. Orito</a>, <a href="/search/?searchtype=author&query=Ormes%2C+J+F">J. F. Ormes</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Seo%2C+E+S">E. S. Seo</a>, <a href="/search/?searchtype=author&query=Shikaze%2C+Y">Y. Shikaze</a>, <a href="/search/?searchtype=author&query=Streitmatter%2C+R+E">R. E. Streitmatter</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+J">J. Suzuki</a>, <a href="/search/?searchtype=author&query=Tanaka%2C+K">K. Tanaka</a>, <a href="/search/?searchtype=author&query=Tanizaki%2C+K">K. Tanizaki</a>, <a href="/search/?searchtype=author&query=Yamagami%2C+T">T. Yamagami</a>, <a href="/search/?searchtype=author&query=Yamamoto%2C+A">A. Yamamoto</a>, <a href="/search/?searchtype=author&query=Yamamoto%2C+Y">Y. Yamamoto</a>, <a href="/search/?searchtype=author&query=Yamato%2C+K">K. Yamato</a>, <a href="/search/?searchtype=author&query=Yoshida%2C+T">T. Yoshida</a> , et al. (1 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="astro-ph/0504361v2-abstract-short" style="display: inline;"> We performed a search for cosmic-ray antideuterons using data collected during four BESS balloon flights from 1997 to 2000. No candidate was found. We derived, for the first time, an upper limit of 1.9E-4 (m^2 s sr GeV/nucleon)^(-1) for the differential flux of cosmic-ray antideuterons, at the 95% confidence level, between 0.17 and 1.15 GeV/nucleon at the top of the atmosphere. </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0504361v2-abstract-full" style="display: none;"> We performed a search for cosmic-ray antideuterons using data collected during four BESS balloon flights from 1997 to 2000. No candidate was found. We derived, for the first time, an upper limit of 1.9E-4 (m^2 s sr GeV/nucleon)^(-1) for the differential flux of cosmic-ray antideuterons, at the 95% confidence level, between 0.17 and 1.15 GeV/nucleon at the top of the atmosphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0504361v2-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0504361v2-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> 6 July, 2005; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 April, 2005; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2005. </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, submitted to Phys. Rev. Lett</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.Lett.95:081101,2005 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/hep-th/0404121">arXiv:hep-th/0404121</a> <span> [<a href="https://arxiv.org/pdf/hep-th/0404121">pdf</a>, <a href="https://arxiv.org/ps/hep-th/0404121">ps</a>, <a href="https://arxiv.org/format/hep-th/0404121">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-th</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</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/10.1142/S0217751X06031399">10.1142/S0217751X06031399 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmological Constant Probing Shape Moduli through Large Extra Dimensions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Matsuda%2C+S">Satoshi Matsuda</a>, <a href="/search/?searchtype=author&query=Seki%2C+S">Shigenori Seki</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="hep-th/0404121v5-abstract-short" style="display: inline;"> We consider compactification of extra dimensions and numerically calculate Casimir energy which is provided by the mass of Kaluza-Klein modes. For the extra space we consider a torus with shape moduli and show that the corresponding vacuum energy is represented as a function of the moduli parameter of the extra dimensions. By assuming that the Casimir energy may be identified with cosmological c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-th/0404121v5-abstract-full').style.display = 'inline'; document.getElementById('hep-th/0404121v5-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-th/0404121v5-abstract-full" style="display: none;"> We consider compactification of extra dimensions and numerically calculate Casimir energy which is provided by the mass of Kaluza-Klein modes. For the extra space we consider a torus with shape moduli and show that the corresponding vacuum energy is represented as a function of the moduli parameter of the extra dimensions. By assuming that the Casimir energy may be identified with cosmological constant, we evaluate the size of extra dimensions in terms of the recent data given by the WMAP observation. We suggest that the observed cosmological constant may probe the shape moduli of the extra space by the study of the Casimir energy of the compactified extra dimensions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-th/0404121v5-abstract-full').style.display = 'none'; document.getElementById('hep-th/0404121v5-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, 2006; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 April, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2004. </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">18 pages, 5 figures, minor corrections, refs. added and corrected</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> KUNS-1857 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Int.J.Mod.Phys. A21 (2006) 3095-3110 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0403704">arXiv:astro-ph/0403704</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0403704">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0403704">ps</a>, <a href="https://arxiv.org/format/astro-ph/0403704">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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.2004.05.019">10.1016/j.physletb.2004.05.019 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurements of Primary and Atmospheric Cosmic-Ray Spectra with the BESS-TeV Spectrometer </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Haino%2C+S">S. Haino</a>, <a href="/search/?searchtype=author&query=Sanuki%2C+T">T. Sanuki</a>, <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Anraku%2C+K">K. Anraku</a>, <a href="/search/?searchtype=author&query=Asaoka%2C+Y">Y. Asaoka</a>, <a href="/search/?searchtype=author&query=Fuke%2C+H">H. Fuke</a>, <a href="/search/?searchtype=author&query=Imori%2C+M">M. Imori</a>, <a href="/search/?searchtype=author&query=Itasaki%2C+A">A. Itasaki</a>, <a href="/search/?searchtype=author&query=Maeno%2C+T">T. Maeno</a>, <a href="/search/?searchtype=author&query=Makida%2C+Y">Y. Makida</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Matsui%2C+N">N. Matsui</a>, <a href="/search/?searchtype=author&query=Matsumoto%2C+H">H. Matsumoto</a>, <a href="/search/?searchtype=author&query=Mitchell%2C+J+W">J. W. Mitchell</a>, <a href="/search/?searchtype=author&query=Moiseev%2C+A+A">A. A. Moiseev</a>, <a href="/search/?searchtype=author&query=Nishimura%2C+J">J. Nishimura</a>, <a href="/search/?searchtype=author&query=Nozaki%2C+M">M. Nozaki</a>, <a href="/search/?searchtype=author&query=Orito%2C+S">S. Orito</a>, <a href="/search/?searchtype=author&query=Ormes%2C+J+F">J. F. Ormes</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Seo%2C+E+S">E. S. Seo</a>, <a href="/search/?searchtype=author&query=Shikaze%2C+Y">Y. Shikaze</a>, <a href="/search/?searchtype=author&query=Streitmatter%2C+R+E">R. E. Streitmatter</a>, <a href="/search/?searchtype=author&query=Suzuki%2C+J">J. Suzuki</a>, <a href="/search/?searchtype=author&query=Takasugi%2C+Y">Y. Takasugi</a> , et al. (8 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="astro-ph/0403704v1-abstract-short" style="display: inline;"> Primary and atmospheric cosmic-ray spectra were precisely measured with the BESS-TeV spectrometer. The spectrometer was upgraded from BESS-98 to achieve seven times higher resolution in momentum measurement. We report absolute fluxes of primary protons and helium nuclei in the energy ranges, 1-540 GeV and 1-250 GeV/n, respectively, and absolute flux of atmospheric muons in the momentum range 0.6… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0403704v1-abstract-full').style.display = 'inline'; document.getElementById('astro-ph/0403704v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0403704v1-abstract-full" style="display: none;"> Primary and atmospheric cosmic-ray spectra were precisely measured with the BESS-TeV spectrometer. The spectrometer was upgraded from BESS-98 to achieve seven times higher resolution in momentum measurement. We report absolute fluxes of primary protons and helium nuclei in the energy ranges, 1-540 GeV and 1-250 GeV/n, respectively, and absolute flux of atmospheric muons in the momentum range 0.6-400 GeV/c. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0403704v1-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0403704v1-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> 31 March, 2004; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2004. </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">26 pages, 9 figures, 3 tables, Submitted to Phys. Lett. B</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Lett.B594:35-46,2004 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/hep-ph/0307361">arXiv:hep-ph/0307361</a> <span> [<a href="https://arxiv.org/pdf/hep-ph/0307361">pdf</a>, <a href="https://arxiv.org/ps/hep-ph/0307361">ps</a>, <a href="https://arxiv.org/format/hep-ph/0307361">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-th</span> </div> </div> <p class="title is-5 mathjax"> Proposal for Generic Size of Large Extra Dimensions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Matsuda%2C+S">Satoshi Matsuda</a>, <a href="/search/?searchtype=author&query=Seki%2C+S">Shigenori Seki</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="hep-ph/0307361v2-abstract-short" style="display: inline;"> In order to resolve the hierarchy problem, large extra dimensions have been introduced, and it has been suggested that the size of extra dimensions is sub-millimeter. On the other hand, we assume in this paper that the cosmological constant comes from the Casimir energy of extra dimensions and estimate the size of extra dimensions in terms of the value of the cosmological constant discovered by… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ph/0307361v2-abstract-full').style.display = 'inline'; document.getElementById('hep-ph/0307361v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-ph/0307361v2-abstract-full" style="display: none;"> In order to resolve the hierarchy problem, large extra dimensions have been introduced, and it has been suggested that the size of extra dimensions is sub-millimeter. On the other hand, we assume in this paper that the cosmological constant comes from the Casimir energy of extra dimensions and estimate the size of extra dimensions in terms of the value of the cosmological constant discovered by the recent WMAP observations. We demonstrate that this size is consistent with the one derived from the hierarchy problem and propose that there may be a generic size of large extra dimensions when the number of extra dimensions is equal to two. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ph/0307361v2-abstract-full').style.display = 'none'; document.getElementById('hep-ph/0307361v2-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 August, 2003; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 July, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">7 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> KUNS-1849 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0304102">arXiv:astro-ph/0304102</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0304102">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0304102">ps</a>, <a href="https://arxiv.org/format/astro-ph/0304102">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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/S0370-2693(03)00676-2">10.1016/S0370-2693(03)00676-2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurements of Proton, Helium and Muon Spectra at Small Atmospheric Depths with the BESS Spectrometer </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Sanuki%2C+T">T. Sanuki</a>, <a href="/search/?searchtype=author&query=Anraku%2C+K">K. Anraku</a>, <a href="/search/?searchtype=author&query=Asaoka%2C+Y">Y. Asaoka</a>, <a href="/search/?searchtype=author&query=Fuke%2C+H">H. Fuke</a>, <a href="/search/?searchtype=author&query=Haino%2C+S">S. Haino</a>, <a href="/search/?searchtype=author&query=Ikeda%2C+N">N. Ikeda</a>, <a href="/search/?searchtype=author&query=Imori%2C+M">M. Imori</a>, <a href="/search/?searchtype=author&query=Izumi%2C+K">K. Izumi</a>, <a href="/search/?searchtype=author&query=Maeno%2C+T">T. Maeno</a>, <a href="/search/?searchtype=author&query=Makida%2C+Y">Y. Makida</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Matsui%2C+N">N. Matsui</a>, <a href="/search/?searchtype=author&query=Matsukawa%2C+T">T. Matsukawa</a>, <a href="/search/?searchtype=author&query=Matsumoto%2C+H">H. Matsumoto</a>, <a href="/search/?searchtype=author&query=Mitchell%2C+J+W">J. W. Mitchell</a>, <a href="/search/?searchtype=author&query=Moiseev%2C+A+A">A. A. Moiseev</a>, <a href="/search/?searchtype=author&query=Nishimura%2C+J">J. Nishimura</a>, <a href="/search/?searchtype=author&query=Nozaki%2C+M">M. Nozaki</a>, <a href="/search/?searchtype=author&query=Orito%2C+S">S. Orito</a>, <a href="/search/?searchtype=author&query=Ormes%2C+J+F">J. F. Ormes</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+M">M. Sasaki</a>, <a href="/search/?searchtype=author&query=Seo%2C+E+S">E. S. Seo</a>, <a href="/search/?searchtype=author&query=Shikaze%2C+Y">Y. Shikaze</a>, <a href="/search/?searchtype=author&query=Sonoda%2C+T">T. Sonoda</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="astro-ph/0304102v2-abstract-short" style="display: inline;"> The cosmic-ray proton, helium, and muon spectra at small atmospheric depths of 4.5 -- 28 g/cm^2 were precisely measured during the slow descending period of the BESS-2001 balloon flight. The variation of atmospheric secondary particle fluxes as a function of atmospheric depth provides fundamental information to study hadronic interactions of the primary cosmic rays with the atmosphere. </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0304102v2-abstract-full" style="display: none;"> The cosmic-ray proton, helium, and muon spectra at small atmospheric depths of 4.5 -- 28 g/cm^2 were precisely measured during the slow descending period of the BESS-2001 balloon flight. The variation of atmospheric secondary particle fluxes as a function of atmospheric depth provides fundamental information to study hadronic interactions of the primary cosmic rays with the atmosphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0304102v2-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0304102v2-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> 6 May, 2003; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 April, 2003; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">21 pages, 11 figures, 4 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Lett. B564 (2003) 8-20; Erratum-ibid. B645 (2007) 472-475 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/astro-ph/0109007">arXiv:astro-ph/0109007</a> <span> [<a href="https://arxiv.org/pdf/astro-ph/0109007">pdf</a>, <a href="https://arxiv.org/ps/astro-ph/0109007">ps</a>, <a href="https://arxiv.org/format/astro-ph/0109007">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics">astro-ph</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.88.051101">10.1103/PhysRevLett.88.051101 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurements of Cosmic-ray Low-energy Antiproton and Proton Spectra in a Transient Period of the Solar Field Reversal </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Asaoka%2C+Y">Y. Asaoka</a>, <a href="/search/?searchtype=author&query=Shikaze%2C+Y">Y. Shikaze</a>, <a href="/search/?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/?searchtype=author&query=Anraku%2C+K">K. Anraku</a>, <a href="/search/?searchtype=author&query=Fujikawa%2C+M">M. Fujikawa</a>, <a href="/search/?searchtype=author&query=Fuke%2C+H">H. Fuke</a>, <a href="/search/?searchtype=author&query=Haino%2C+S">S. Haino</a>, <a href="/search/?searchtype=author&query=Imori%2C+M">M. Imori</a>, <a href="/search/?searchtype=author&query=Izumi%2C+K">K. Izumi</a>, <a href="/search/?searchtype=author&query=Maeno%2C+T">T. Maeno</a>, <a href="/search/?searchtype=author&query=Makida%2C+Y">Y. Makida</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">S. Matsuda</a>, <a href="/search/?searchtype=author&query=Matsui%2C+N">N. Matsui</a>, <a href="/search/?searchtype=author&query=Matsukawa%2C+T">T. Matsukawa</a>, <a href="/search/?searchtype=author&query=Matsumoto%2C+H">H. Matsumoto</a>, <a href="/search/?searchtype=author&query=Matsunaga%2C+H">H. Matsunaga</a>, <a href="/search/?searchtype=author&query=Mitchell%2C+J">J. Mitchell</a>, <a href="/search/?searchtype=author&query=Mitsui%2C+T">T. Mitsui</a>, <a href="/search/?searchtype=author&query=Moiseev%2C+A">A. Moiseev</a>, <a href="/search/?searchtype=author&query=Motoki%2C+M">M. Motoki</a>, <a href="/search/?searchtype=author&query=Nishimura%2C+J">J. Nishimura</a>, <a href="/search/?searchtype=author&query=Nozaki%2C+M">M. Nozaki</a>, <a href="/search/?searchtype=author&query=Orito%2C+S">S. Orito</a>, <a href="/search/?searchtype=author&query=Ormes%2C+J+F">J. F. Ormes</a>, <a href="/search/?searchtype=author&query=Saeki%2C+T">T. Saeki</a> , et al. (17 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="astro-ph/0109007v2-abstract-short" style="display: inline;"> The energy spectra of cosmic-ray low-energy antiprotons and protons have been measured by BESS in 1999 and 2000, during a period covering the solar magnetic field reversal. Based on these measurements, a sudden increase of the antiproton to proton flux ratio following the solar magnetic field reversal was observed, and it generally agrees with a drift model of the solar modulation. </span> <span class="abstract-full has-text-grey-dark mathjax" id="astro-ph/0109007v2-abstract-full" style="display: none;"> The energy spectra of cosmic-ray low-energy antiprotons and protons have been measured by BESS in 1999 and 2000, during a period covering the solar magnetic field reversal. Based on these measurements, a sudden increase of the antiproton to proton flux ratio following the solar magnetic field reversal was observed, and it generally agrees with a drift model of the solar modulation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('astro-ph/0109007v2-abstract-full').style.display = 'none'; document.getElementById('astro-ph/0109007v2-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 January, 2002; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 September, 2001; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2001. </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, 4 figures, revised version accepted for publication in Phys. Rev. Lett</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.Lett.88:051101,2002 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/hep-th/0105080">arXiv:hep-th/0105080</a> <span> [<a href="https://arxiv.org/pdf/hep-th/0105080">pdf</a>, <a href="https://arxiv.org/ps/hep-th/0105080">ps</a>, <a href="https://arxiv.org/format/hep-th/0105080">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-th</span> </div> </div> <p class="title is-5 mathjax"> Gravitational Stability and Screening Effect from Extra Timelike Dimensions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Matsuda%2C+S">Satoshi Matsuda</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="hep-th/0105080v2-abstract-short" style="display: inline;"> We discuss extra timelike dimensions and their effects on the gravitational stability of spherical massive bodies. Here we specifically report our results for the case of one extra timelike dimension where we have made analytically rigorous investigations on the tachyonic graviton exchange due to the infinite tower of the Kaluza-Klein mode. With the scale $L$ of the extra timelike dimension we f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-th/0105080v2-abstract-full').style.display = 'inline'; document.getElementById('hep-th/0105080v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-th/0105080v2-abstract-full" style="display: none;"> We discuss extra timelike dimensions and their effects on the gravitational stability of spherical massive bodies. Here we specifically report our results for the case of one extra timelike dimension where we have made analytically rigorous investigations on the tachyonic graviton exchange due to the infinite tower of the Kaluza-Klein mode. With the scale $L$ of the extra timelike dimension we find that some spherical bodies of radius $R$ can be stable at critical radii $R=2蟺Lp$ for some positive integer $p$. We also obtain the generic property of massive bodies that for the short distance range $0<R\leq 蟺L$ the gravitational force due to the ordinary massless graviton exchange is screened by the Kaluza-Klein mode exchange of tachyonic gravitons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-th/0105080v2-abstract-full').style.display = 'none'; document.getElementById('hep-th/0105080v2-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> 10 May, 2001; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 May, 2001; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2001. </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, based on the invited talk at the XXXVIth Rencontres de Moriond, to appear in proceedings. Typos corrected</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> KUCP-0181 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/hep-th/0008216">arXiv:hep-th/0008216</a> <span> [<a href="https://arxiv.org/pdf/hep-th/0008216">pdf</a>, <a href="https://arxiv.org/ps/hep-th/0008216">ps</a>, <a href="https://arxiv.org/format/hep-th/0008216">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-th</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</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/S0550-3213(00)00776-8">10.1016/S0550-3213(00)00776-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gravitational Stability and Screening Effect from D Extra Timelike Dimensions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Matsuda%2C+S">Satoshi Matsuda</a>, <a href="/search/?searchtype=author&query=Seki%2C+S">Shigenori Seki</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="hep-th/0008216v3-abstract-short" style="display: inline;"> We study (3+1)+D dimensional spacetime, where D extra dimensions are timelike. Compactification of the D timelike dimensions leads to tachyonic Kaluza-Klein gravitons. We calculate the gravitational self-energies of massive spherical bodies due to the tachyonic exchange, discuss their stability, and find that the gravitational force is screened in a certain number of the extra dimensions. We als… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-th/0008216v3-abstract-full').style.display = 'inline'; document.getElementById('hep-th/0008216v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-th/0008216v3-abstract-full" style="display: none;"> We study (3+1)+D dimensional spacetime, where D extra dimensions are timelike. Compactification of the D timelike dimensions leads to tachyonic Kaluza-Klein gravitons. We calculate the gravitational self-energies of massive spherical bodies due to the tachyonic exchange, discuss their stability, and find that the gravitational force is screened in a certain number of the extra dimensions. We also derive the exact relationship between the Newton constants in the full 4+D dimensional spacetime with the D extra times and the ordinary Newton constant of our 4 dimensional world. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-th/0008216v3-abstract-full').style.display = 'none'; document.getElementById('hep-th/0008216v3-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, 2000; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 August, 2000; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2000. </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">harvmac, 20 pages, typos corrected, refs. added and corrected</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> KUCP-0166 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl.Phys. B599 (2001) 119-136 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/hep-ph/0007290">arXiv:hep-ph/0007290</a> <span> [<a href="https://arxiv.org/pdf/hep-ph/0007290">pdf</a>, <a href="https://arxiv.org/ps/hep-ph/0007290">ps</a>, <a href="https://arxiv.org/format/hep-ph/0007290">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-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/10.1103/PhysRevD.63.065014">10.1103/PhysRevD.63.065014 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </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/PhysRevD.63.129901">10.1103/PhysRevD.63.129901 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gravitational Stability and Extra Timelike Dimensions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Matsuda%2C+S">Satoshi Matsuda</a>, <a href="/search/?searchtype=author&query=Seki%2C+S">Shigenori Seki</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="hep-ph/0007290v3-abstract-short" style="display: inline;"> Tachyonic Kaluza-Klein modes normally appear from the compactification of extra timelike dimensions with scale $L$ and lead to some instabilities of physical systems. We calculate the contribution of tachyonic gravitons to the self energies of spherical massive bodies of radius $R$ and discuss their possible gravitational stability. We find that some spherical bodies can be stable at critical ra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ph/0007290v3-abstract-full').style.display = 'inline'; document.getElementById('hep-ph/0007290v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-ph/0007290v3-abstract-full" style="display: none;"> Tachyonic Kaluza-Klein modes normally appear from the compactification of extra timelike dimensions with scale $L$ and lead to some instabilities of physical systems. We calculate the contribution of tachyonic gravitons to the self energies of spherical massive bodies of radius $R$ and discuss their possible gravitational stability. We find that some spherical bodies can be stable at critical radii $R=2蟺L p$ for some positive integers $p$. We also prove the generic property of massive bodies that for the range $0<R\leq蟺L$ the gravitational force due to the ordinary massless graviton exchange is screened by the Kaluza-Klein mode exchange of tachyonic gravitons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ph/0007290v3-abstract-full').style.display = 'none'; document.getElementById('hep-ph/0007290v3-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> 5 August, 2000; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 July, 2000; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2000. </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">harvmac, 10 pages, 4 figures; typos corrected, one comment and ref.[5] added</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.D63:065014,2001; Erratum-ibid.D63:129901,2001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/hep-ph/9802342">arXiv:hep-ph/9802342</a> <span> [<a href="https://arxiv.org/pdf/hep-ph/9802342">pdf</a>, <a href="https://arxiv.org/ps/hep-ph/9802342">ps</a>, <a href="https://arxiv.org/format/hep-ph/9802342">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Concluding Remarks - International Symposium on ``QCD Corrections and New Physics", 1997, Hiroshima, Japan - </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Matsuda%2C+S">Satoshi Matsuda</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="hep-ph/9802342v1-abstract-short" style="display: inline;"> This is a report of the concluding talk presented at the International Symposium on QCD Corrections and New Physics which was held during October 27-29, 1997 at Mielparque Hiroshima, Hiroshima, Japan. The report will be published in the Conference Proceedings. </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-ph/9802342v1-abstract-full" style="display: none;"> This is a report of the concluding talk presented at the International Symposium on QCD Corrections and New Physics which was held during October 27-29, 1997 at Mielparque Hiroshima, Hiroshima, Japan. The report will be published in the Conference Proceedings. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ph/9802342v1-abstract-full').style.display = 'none'; document.getElementById('hep-ph/9802342v1-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> 17 February, 1998; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 1998. </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, LaTeX file</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> KUCP-0112 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/hep-th/9610212">arXiv:hep-th/9610212</a> <span> [<a href="https://arxiv.org/pdf/hep-th/9610212">pdf</a>, <a href="https://arxiv.org/ps/hep-th/9610212">ps</a>, <a href="https://arxiv.org/format/hep-th/9610212">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-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/10.1142/S0217751X97002516">10.1142/S0217751X97002516 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectral Flow and Feigin-Fuks Parameter Space of N=4 Superconformal Algebras </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Matsuda%2C+S">Satoshi Matsuda</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="hep-th/9610212v1-abstract-short" style="display: inline;"> The parameter space of the Feigin-Fuks representations of the N=4 SU(2)$_k$ superconformal algebras is studied from the viewpoint of the specral flow. The $畏$ phase of the spectral flow is nicely incorporated through twisted fermions and the spectral flow resulting from the inner automorphism of the N=4 superconformal algebras is explicitly shown to be operating as identiy relations among the ge… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-th/9610212v1-abstract-full').style.display = 'inline'; document.getElementById('hep-th/9610212v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-th/9610212v1-abstract-full" style="display: none;"> The parameter space of the Feigin-Fuks representations of the N=4 SU(2)$_k$ superconformal algebras is studied from the viewpoint of the specral flow. The $畏$ phase of the spectral flow is nicely incorporated through twisted fermions and the spectral flow resulting from the inner automorphism of the N=4 superconformal algebras is explicitly shown to be operating as identiy relations among the generators. Conditions for the unitary representations are also investigated in our Feigin-Fuks parameter space. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-th/9610212v1-abstract-full').style.display = 'none'; document.getElementById('hep-th/9610212v1-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> 28 October, 1996; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 1996. </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">LaTeX file, 21 pages, 1 figure(ps file)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> KUCP-102 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Int.J.Mod.Phys. A12 (1997) 4707-4724 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/hep-th/9609184">arXiv:hep-th/9609184</a> <span> [<a href="https://arxiv.org/pdf/hep-th/9609184">pdf</a>, <a href="https://arxiv.org/ps/hep-th/9609184">ps</a>, <a href="https://arxiv.org/format/hep-th/9609184">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-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/10.1142/S0217732396002617">10.1142/S0217732396002617 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Feigin-Fuchs Representations for Nonequivalent Algebras of N=4 Superconformal Symmetery </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Matsuda%2C+S">Satoshi Matsuda</a>, <a href="/search/?searchtype=author&query=Ishimoto%2C+Y">Yukitaka Ishimoto</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="hep-th/9609184v1-abstract-short" style="display: inline;"> The $N=4$ SU(2)$_k$ superconformal algebra has the global automorphism of SO(4) $\approx$ SU(2)$\times$SU(2) with the {\it left} factor as the Kac-Moody gauge symmetry. As a consequence, an infinite set of independent algebras labeled by $蟻$ corresponding to the conjugate classes of the {\it outer} automorphism group SO(4)/SU(2)=SU(2) are obtained 脿 la Schwimmer and Seiberg. We construct Feigin-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-th/9609184v1-abstract-full').style.display = 'inline'; document.getElementById('hep-th/9609184v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-th/9609184v1-abstract-full" style="display: none;"> The $N=4$ SU(2)$_k$ superconformal algebra has the global automorphism of SO(4) $\approx$ SU(2)$\times$SU(2) with the {\it left} factor as the Kac-Moody gauge symmetry. As a consequence, an infinite set of independent algebras labeled by $蟻$ corresponding to the conjugate classes of the {\it outer} automorphism group SO(4)/SU(2)=SU(2) are obtained 脿 la Schwimmer and Seiberg. We construct Feigin-Fuchs representations with the $蟻$ parameter embedded for the infinite set of the $N=4$ nonequivalent algebras. In our construction the extended global SU(2) algebras labeled by $蟻$ are self-consistently represented by fermion fields with appropriate boundary conditions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-th/9609184v1-abstract-full').style.display = 'none'; document.getElementById('hep-th/9609184v1-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 September, 1996; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 1996. </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">19 pages, LaTeX file</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> KUCP-101 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Mod.Phys.Lett. A11 (1996) 2611-2624 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/hep-ph/9408353">arXiv:hep-ph/9408353</a> <span> [<a href="https://arxiv.org/pdf/hep-ph/9408353">pdf</a>, <a href="https://arxiv.org/ps/hep-ph/9408353">ps</a>, <a href="https://arxiv.org/format/hep-ph/9408353">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</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/10.1016/0370-2693(94)01648-V">10.1016/0370-2693(94)01648-V <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> More on the Burkhardt-Cottingham Sum Rule in QCD </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kodaira%2C+J">Jiro Kodaira</a>, <a href="/search/?searchtype=author&query=Matsuda%2C+S">Satoshi Matsuda</a>, <a href="/search/?searchtype=author&query=Uematsu%2C+T">Tsuneo Uematsu</a>, <a href="/search/?searchtype=author&query=Sasaki%2C+K">Ken Sasaki</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="hep-ph/9408353v1-abstract-short" style="display: inline;"> The QCD higher order effects to the polarized structure function $g_2(x, Q^2 )$ are reanalyzed for massive quarks in the context of the operator product expansion. We confirm that the lowest moment of $g_2 (x, Q^2 )$ which corresponds to the Burkhardt-Cottingham sum rule does {\sl not} suffer from radiative corrections in perturbative QCD. </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-ph/9408353v1-abstract-full" style="display: none;"> The QCD higher order effects to the polarized structure function $g_2(x, Q^2 )$ are reanalyzed for massive quarks in the context of the operator product expansion. We confirm that the lowest moment of $g_2 (x, Q^2 )$ which corresponds to the Burkhardt-Cottingham sum rule does {\sl not} suffer from radiative corrections in perturbative QCD. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-ph/9408353v1-abstract-full').style.display = 'none'; document.getElementById('hep-ph/9408353v1-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 August, 1994; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 1994. </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">LaTeX, 9 pages, 1 figure appended after \end{document} as an uu-encoded and compressed .ps file, KUCP-70;HUPD-9410;YNU-HEPTh-94-105</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Lett. B345 (1995) 527-531 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/hep-th/9403035">arXiv:hep-th/9403035</a> <span> [<a href="https://arxiv.org/pdf/hep-th/9403035">pdf</a>, <a href="https://arxiv.org/ps/hep-th/9403035">ps</a>, <a href="https://arxiv.org/format/hep-th/9403035">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-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/10.1142/S0217751X95000802">10.1142/S0217751X95000802 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Representation Blocks of Conformal Fields for the $N$=4 SU(2)$_k$ Superconformal Algebras </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Matsuda%2C+S">Satoshi Matsuda</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="hep-th/9403035v1-abstract-short" style="display: inline;"> The representation theories of the SU(2)$_k$-extended $N$=4 superconformal algebras (SCAs) with $arbitrary$ level $k$ are developed being based on their Feigin-Fuchs representations found recently by the present author. A basic unit of the representation blocks consisting of eight \lq\lq boson-like\rq\rq\ and eight \lq\lq fermion-like\rq\rq\ conformal fields is found to describe arbitrary repres… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-th/9403035v1-abstract-full').style.display = 'inline'; document.getElementById('hep-th/9403035v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-th/9403035v1-abstract-full" style="display: none;"> The representation theories of the SU(2)$_k$-extended $N$=4 superconformal algebras (SCAs) with $arbitrary$ level $k$ are developed being based on their Feigin-Fuchs representations found recently by the present author. A basic unit of the representation blocks consisting of eight \lq\lq boson-like\rq\rq\ and eight \lq\lq fermion-like\rq\rq\ conformal fields is found to describe arbitrary representations of the $N$=4 SU(2)$_k$ SCAs, including {\it unitary} and {\it nonunitary} representations. The transformation properties of the fundamental sets of the conformal fields under the $N$=4 SU(2)$_k$ superconformal symmetries are given. Then, the whole sets of the charge-screening operators of the $N$=4 SU(2)$_k$ SCAs are identified out of the sixteen conformal fields in the basic unit of the representation blocks. The conditions for the {\it eligible} charge-screening operators are analyzed in terms of the continuous parameters which enter in our vertex-operator forms for the fundamental conformal fields of the representation blocks. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-th/9403035v1-abstract-full').style.display = 'none'; document.getElementById('hep-th/9403035v1-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> 6 March, 1994; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 1994. </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">30 pages, KUCP-64, phyzzx, TeX file</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Int.J.Mod.Phys. A10 (1995) 1671-1692 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/hep-th/9201008">arXiv:hep-th/9201008</a> <span> [<a href="https://arxiv.org/pdf/hep-th/9201008">pdf</a>, <a href="https://arxiv.org/ps/hep-th/9201008">ps</a>, <a href="https://arxiv.org/format/hep-th/9201008">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-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/10.1016/0370-2693(92)90479-N">10.1016/0370-2693(92)90479-N <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Coulomb Gas Representations and Screening Operators of the N=4 Superconformal Algebras </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Matsuda%2C+S">Satoshi Matsuda</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="hep-th/9201008v1-abstract-short" style="display: inline;"> The Coulomb gas representations are presented for the ${\rm SU(2)}$$_k$-extended $N$=4 superconformal algebras, incorporating the Feigin-Fuchs representation of the\break ${\rm SU(2)}$$_k$ Kac-Moody algebra with {\sl arbitrary} level $k$. Then the long-standing problem of identifying the whole set of charge-screening operators for the $N$=4 superconformal algebras is solved and their explicit ex… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-th/9201008v1-abstract-full').style.display = 'inline'; document.getElementById('hep-th/9201008v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="hep-th/9201008v1-abstract-full" style="display: none;"> The Coulomb gas representations are presented for the ${\rm SU(2)}$$_k$-extended $N$=4 superconformal algebras, incorporating the Feigin-Fuchs representation of the\break ${\rm SU(2)}$$_k$ Kac-Moody algebra with {\sl arbitrary} level $k$. Then the long-standing problem of identifying the whole set of charge-screening operators for the $N$=4 superconformal algebras is solved and their explicit expressions are given. The method of achieving a rigorous proof of the $N$=4 Kac determinant formulae following Kato and Matsuda is suggested. The complete proof for them will be given elsewhere. Our results for the screening operators also provide the basis for studying the BRST formalism of the $N$=4 superconformal algebras ${\sl {\grave a}\ la}$ Felder. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('hep-th/9201008v1-abstract-full').style.display = 'none'; document.getElementById('hep-th/9201008v1-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> 7 January, 1992; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 1992. </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</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Lett. B282 (1992) 56-62 </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