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 1–21 of 21 results for author: <span class="mathjax">Bottai, 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/physics" aria-role="search"> Searching in archive <strong>physics</strong>. <a href="/search/?searchtype=author&query=Bottai%2C+S">Search in all archives.</a> <div class="field has-addons-tablet"> <div class="control is-expanded"> <label for="query" class="hidden-label">Search term or terms</label> <input class="input is-medium" id="query" name="query" placeholder="Search term..." type="text" value="Bottai, 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=Bottai%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="Bottai, 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/2410.03274">arXiv:2410.03274</a> <span> [<a href="https://arxiv.org/pdf/2410.03274">pdf</a>, <a href="https://arxiv.org/format/2410.03274">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"> Performance assessment of the HERD calorimeter with a photo-diode read-out system for high-energy electron beams </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+M">M. Antonelli</a>, <a href="/search/physics?searchtype=author&query=Bai%2C+Y">Y. Bai</a>, <a href="/search/physics?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/physics?searchtype=author&query=Bao%2C+T">T. Bao</a>, <a href="/search/physics?searchtype=author&query=Barbanera%2C+M">M. Barbanera</a>, <a href="/search/physics?searchtype=author&query=Berti%2C+E">E. Berti</a>, <a href="/search/physics?searchtype=author&query=Betti%2C+P">P. Betti</a>, <a href="/search/physics?searchtype=author&query=Bigongiari%2C+G">G. Bigongiari</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Cagnoli%2C+I">I. Cagnoli</a>, <a href="/search/physics?searchtype=author&query=Cao%2C+W">W. Cao</a>, <a href="/search/physics?searchtype=author&query=Casaus%2C+J">J. Casaus</a>, <a href="/search/physics?searchtype=author&query=Cerasole%2C+D">D. Cerasole</a>, <a href="/search/physics?searchtype=author&query=Chen%2C+Z">Z. Chen</a>, <a href="/search/physics?searchtype=author&query=Cui%2C+X">X. Cui</a>, <a href="/search/physics?searchtype=author&query=D%27Alessandro%2C+R">R. D'Alessandro</a>, <a href="/search/physics?searchtype=author&query=Di+Venere%2C+L">L. Di Venere</a>, <a href="/search/physics?searchtype=author&query=Diaz%2C+C">C. Diaz</a>, <a href="/search/physics?searchtype=author&query=Dong%2C+Y">Y. Dong</a>, <a href="/search/physics?searchtype=author&query=Detti%2C+S">S. Detti</a>, <a href="/search/physics?searchtype=author&query=Duranti%2C+M">M. Duranti</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="2410.03274v1-abstract-short" style="display: inline;"> The measurement of cosmic rays at energies exceeding 100 TeV per nucleon is crucial for enhancing the understanding of high-energy particle propagation and acceleration models in the Galaxy. HERD is a space-borne calorimetric experiment that aims to extend the current direct measurements of cosmic rays to unexplored energies. The payload is scheduled to be installed on the Chinese Space Station in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.03274v1-abstract-full').style.display = 'inline'; document.getElementById('2410.03274v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.03274v1-abstract-full" style="display: none;"> The measurement of cosmic rays at energies exceeding 100 TeV per nucleon is crucial for enhancing the understanding of high-energy particle propagation and acceleration models in the Galaxy. HERD is a space-borne calorimetric experiment that aims to extend the current direct measurements of cosmic rays to unexplored energies. The payload is scheduled to be installed on the Chinese Space Station in 2027. The primary peculiarity of the instrument is its capability to measure particles coming from all directions, with the main detector being a deep, homogeneous, 3D calorimeter. The active elements are read out using two independent systems: one based on wavelength shifter fibers coupled to CMOS cameras, and the other based on photo-diodes read-out with custom front-end electronics. A large calorimeter prototype was tested in 2023 during an extensive beam test campaign at CERN. In this paper, the performance of the calorimeter for high-energy electron beams, as obtained from the photo-diode system data, is presented. The prototype demonstrated excellent performance, e.g., an energy resolution better than 1% for electrons at 250 GeV. A comparison between beam test data and Monte Carlo simulation data is also presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.03274v1-abstract-full').style.display = 'none'; document.getElementById('2410.03274v1-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.04133">arXiv:2208.04133</a> <span> [<a href="https://arxiv.org/pdf/2208.04133">pdf</a>, <a href="https://arxiv.org/format/2208.04133">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 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/10.1088/1748-0221/17/09/P09002">10.1088/1748-0221/17/09/P09002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Development of the photo-diode subsystem for the HERD calorimeter double-readout </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+M">M. Antonelli</a>, <a href="/search/physics?searchtype=author&query=Basti%2C+A">A. Basti</a>, <a href="/search/physics?searchtype=author&query=Berti%2C+E">E. Berti</a>, <a href="/search/physics?searchtype=author&query=Betti%2C+P">P. Betti</a>, <a href="/search/physics?searchtype=author&query=Bigongiari%2C+G">G. Bigongiari</a>, <a href="/search/physics?searchtype=author&query=Bonechi%2C+L">L. Bonechi</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Brogi%2C+P">P. Brogi</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Checchia%2C+C">C. Checchia</a>, <a href="/search/physics?searchtype=author&query=Casaus%2C+J">J. Casaus</a>, <a href="/search/physics?searchtype=author&query=Cui%2C+X">X. Cui</a>, <a href="/search/physics?searchtype=author&query=Dong%2C+Y">Y. Dong</a>, <a href="/search/physics?searchtype=author&query=D%27Alessandro%2C+R">R. D'Alessandro</a>, <a href="/search/physics?searchtype=author&query=Detti%2C+S">S. Detti</a>, <a href="/search/physics?searchtype=author&query=Giovacchini%2C+F">F. Giovacchini</a>, <a href="/search/physics?searchtype=author&query=Finetti%2C+N">N. Finetti</a>, <a href="/search/physics?searchtype=author&query=Maestro%2C+P">P. Maestro</a>, <a href="/search/physics?searchtype=author&query=Marrocchesi%2C+P+S">P. S. Marrocchesi</a>, <a href="/search/physics?searchtype=author&query=Liu%2C+X">X. Liu</a>, <a href="/search/physics?searchtype=author&query=Marin%2C+J">J. Marin</a>, <a href="/search/physics?searchtype=author&query=Martinez%2C+G">G. Martinez</a> , et al. (18 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="2208.04133v1-abstract-short" style="display: inline;"> The measurement of cosmic-ray individual spectra provides unique information regarding the origin and propagation of astro-particles. Due to the limited acceptance of current space experiments, protons and nuclei around the "knee" region ($\sim1\ PeV$) can only be observed by ground based experiments. Thanks to an innovative design, the High Energy cosmic-Radiation Detection (HERD) facility will a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.04133v1-abstract-full').style.display = 'inline'; document.getElementById('2208.04133v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.04133v1-abstract-full" style="display: none;"> The measurement of cosmic-ray individual spectra provides unique information regarding the origin and propagation of astro-particles. Due to the limited acceptance of current space experiments, protons and nuclei around the "knee" region ($\sim1\ PeV$) can only be observed by ground based experiments. Thanks to an innovative design, the High Energy cosmic-Radiation Detection (HERD) facility will allow direct observation up to this energy region: the instrument is mainly based on a 3D segmented, isotropic and homogeneous calorimeter which properly measures the energy of particles coming from each direction and it will be made of about 7500 LYSO cubic crystals. The read-out of the scintillation light is done with two independent systems: the first one based on wave-length shifting fibers coupled to Intensified scientific CMOS cameras, the second one is made of two photo-diodes with different active areas connected to a custom front-end electronics. This photo-diode system is designed to achieve a huge dynamic range, larger than $10^7$, while having a small power consumption, few mW per channel. Thanks to a good signal-to-noise ratio, the capability of a proper calibration, by using signals of both non-interacting and showering particles, is also guaranteed. In this paper, the current design and the performance obtained by several tests of the photo-diode read-out system are discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.04133v1-abstract-full').style.display = 'none'; document.getElementById('2208.04133v1-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 17 P09002 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.10327">arXiv:2110.10327</a> <span> [<a href="https://arxiv.org/pdf/2110.10327">pdf</a>, <a href="https://arxiv.org/format/2110.10327">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="Applied Physics">physics.app-ph</span> </div> </div> <p class="title is-5 mathjax"> BLEMAB European project: muon imaging technique applied to blast furnaces </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=BLEMAB+Collaboration"> BLEMAB Collaboration</a>, <a href="/search/physics?searchtype=author&query=Bonechi%2C+L">L. Bonechi</a>, <a href="/search/physics?searchtype=author&query=Ambrosino%2C+F">F. Ambrosino</a>, <a href="/search/physics?searchtype=author&query=Andreetto%2C+P">P. Andreetto</a>, <a href="/search/physics?searchtype=author&query=Bonomi%2C+G">G. Bonomi</a>, <a href="/search/physics?searchtype=author&query=Borselli%2C+D">D. Borselli</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Buhles%2C+T">T. Buhles</a>, <a href="/search/physics?searchtype=author&query=Calliari%2C+I">I. Calliari</a>, <a href="/search/physics?searchtype=author&query=Checchia%2C+P">P. Checchia</a>, <a href="/search/physics?searchtype=author&query=Chiarotti%2C+U">U. Chiarotti</a>, <a href="/search/physics?searchtype=author&query=Cialdai%2C+C">C. Cialdai</a>, <a href="/search/physics?searchtype=author&query=Ciaranfi%2C+R">R. Ciaranfi</a>, <a href="/search/physics?searchtype=author&query=Cimmino%2C+L">L. Cimmino</a>, <a href="/search/physics?searchtype=author&query=Ciulli%2C+V">V. Ciulli</a>, <a href="/search/physics?searchtype=author&query=D%27Alessandro%2C+R">R. D'Alessandro</a>, <a href="/search/physics?searchtype=author&query=D%27Errico%2C+M">M. D'Errico</a>, <a href="/search/physics?searchtype=author&query=Ferretti%2C+R">R. Ferretti</a>, <a href="/search/physics?searchtype=author&query=Finke%2C+F">F. Finke</a>, <a href="/search/physics?searchtype=author&query=Franzen%2C+A">A. Franzen</a>, <a href="/search/physics?searchtype=author&query=Glaser%2C+B">B. Glaser</a>, <a href="/search/physics?searchtype=author&query=Gonzi%2C+S">S. Gonzi</a>, <a href="/search/physics?searchtype=author&query=Liu%2C+Y">Y. Liu</a>, <a href="/search/physics?searchtype=author&query=Lorenzon%2C+A">A. Lorenzon</a>, <a href="/search/physics?searchtype=author&query=Masone%2C+V">V. Masone</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="2110.10327v2-abstract-short" style="display: inline;"> The BLEMAB European project (BLast furnace stack density Estimation through online Muon ABsorption measurements), evolution of the previous MuBlast European project, is designed to investigate in detail the capability of muon radiography techniques applied to the imaging of a blast furnace's inner zone. In particular, the geometry and size of the so called cohesive zone, i.e. the spatial zone wher… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.10327v2-abstract-full').style.display = 'inline'; document.getElementById('2110.10327v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.10327v2-abstract-full" style="display: none;"> The BLEMAB European project (BLast furnace stack density Estimation through online Muon ABsorption measurements), evolution of the previous MuBlast European project, is designed to investigate in detail the capability of muon radiography techniques applied to the imaging of a blast furnace's inner zone. In particular, the geometry and size of the so called cohesive zone, i.e. the spatial zone where the slowly downward moving material begins to soften and melt, that plays an important role in the performance of the blast furnace itself. Thanks to the high penetration power of the natural cosmic ray muon radiation, muon transmission radiography represents an appropriate non-invasive methodology for imaging large high-density structures such as blast furnaces, whose linear size can be up to a few tens of meters. A state-of-the-art muon tracking system, whose design profits from the long experience of our collaboration in this field, is currently under development and will be installed in 2022 at a blast furnace on the ArcelorMittal site in Bremen (Germany) for many months. Collected data will be exploited to monitor temporal variations of the average density distribution inside the furnace. Muon radiography results will also be compared with measurements obtained through an enhanced multipoint probe and standard blast furnace models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.10327v2-abstract-full').style.display = 'none'; document.getElementById('2110.10327v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">12 pages, 15 figures, IWORID 2021 Workshop</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.01561">arXiv:2110.01561</a> <span> [<a href="https://arxiv.org/pdf/2110.01561">pdf</a>, <a href="https://arxiv.org/format/2110.01561">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</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/10.1088/1748-0221/16/10/P10024">10.1088/1748-0221/16/10/P10024 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The CaloCube calorimeter for high-energy cosmic-ray measurements in space: performance of a large-scale prototype </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Agnesi%2C+A">A. Agnesi</a>, <a href="/search/physics?searchtype=author&query=Albergo%2C+S">S. Albergo</a>, <a href="/search/physics?searchtype=author&query=Antonelli%2C+M">M. Antonelli</a>, <a href="/search/physics?searchtype=author&query=Auditore%2C+L">L. Auditore</a>, <a href="/search/physics?searchtype=author&query=Basti%2C+A">A. Basti</a>, <a href="/search/physics?searchtype=author&query=Berti%2C+E">E. Berti</a>, <a href="/search/physics?searchtype=author&query=Bigongiari%2C+G">G. Bigongiari</a>, <a href="/search/physics?searchtype=author&query=Bonechi%2C+L">L. Bonechi</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Brogi%2C+P">P. Brogi</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Cattaneo%2C+P+W">P. W. Cattaneo</a>, <a href="/search/physics?searchtype=author&query=Checchia%2C+C">C. Checchia</a>, <a href="/search/physics?searchtype=author&query=Alessandro%2C+R+D">R. D Alessandro</a>, <a href="/search/physics?searchtype=author&query=Detti%2C+S">S. Detti</a>, <a href="/search/physics?searchtype=author&query=Fasoli%2C+M">M. Fasoli</a>, <a href="/search/physics?searchtype=author&query=Finetti%2C+N">N. Finetti</a>, <a href="/search/physics?searchtype=author&query=Italiano%2C+A">A. Italiano</a>, <a href="/search/physics?searchtype=author&query=Maestro%2C+P">P. Maestro</a>, <a href="/search/physics?searchtype=author&query=Marrocchesi%2C+P+S">P. S. Marrocchesi</a>, <a href="/search/physics?searchtype=author&query=Mori%2C+N">N. Mori</a>, <a href="/search/physics?searchtype=author&query=Orzan%2C+G">G. Orzan</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="2110.01561v1-abstract-short" style="display: inline;"> The direct observation of high-energy cosmic rays, up to the PeV energy region, will increasingly rely on highly performing calorimeters, and the physics performance will be primarily determined by their geometrical acceptance and energy resolution. Thus, it is extremely important to optimize their geometrical design, granularity and absorption depth, with respect to the totalmass of the apparatus… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.01561v1-abstract-full').style.display = 'inline'; document.getElementById('2110.01561v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.01561v1-abstract-full" style="display: none;"> The direct observation of high-energy cosmic rays, up to the PeV energy region, will increasingly rely on highly performing calorimeters, and the physics performance will be primarily determined by their geometrical acceptance and energy resolution. Thus, it is extremely important to optimize their geometrical design, granularity and absorption depth, with respect to the totalmass of the apparatus, which is amongst the most important constraints for a space mission. CaloCube is an homogeneous calorimeter whose basic geometry is cubic and isotropic, obtained by filling the cubic volume with small cubic scintillating crystals. In this way it is possible to detect particles arriving from every direction in space, thus maximizing the acceptance. This design summarizes a three-year R&D activity, aiming to both optimize and study the full-scale performance of the calorimeter, in the perspective of a cosmic-ray space mission, and investigate a viable technical design by means of the construction of several sizable prototypes. A large scale prototype, made of a mesh of 5x5x18 CsI(Tl) crystals, has been constructed and tested on high-energy particle beams at CERN SPS accelerator. In this paper we describe the CaloCube design and present the results relative to the response of the large scale prototype to electrons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.01561v1-abstract-full').style.display = 'none'; document.getElementById('2110.01561v1-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 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">24 pages, 19 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/2008.01390">arXiv:2008.01390</a> <span> [<a href="https://arxiv.org/pdf/2008.01390">pdf</a>, <a href="https://arxiv.org/ps/2008.01390">ps</a>, <a href="https://arxiv.org/format/2008.01390">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 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> </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/10.1088/1748-0221/15/09/P09034">10.1088/1748-0221/15/09/P09034 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Tracker-In-Calorimeter (TIC): a calorimetric approach to tracking gamma rays in space experiments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/physics?searchtype=author&query=Azzarello%2C+P">P. Azzarello</a>, <a href="/search/physics?searchtype=author&query=Basti%2C+A">A. Basti</a>, <a href="/search/physics?searchtype=author&query=Berti%2C+E">E. Berti</a>, <a href="/search/physics?searchtype=author&query=Bertucci%2C+B">B. Bertucci</a>, <a href="/search/physics?searchtype=author&query=Bigongiari%2C+G">G. Bigongiari</a>, <a href="/search/physics?searchtype=author&query=Bonechi%2C+L">L. Bonechi</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Brianzi%2C+M">M. Brianzi</a>, <a href="/search/physics?searchtype=author&query=Brogi%2C+P">P. Brogi</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Catanzani%2C+E">E. Catanzani</a>, <a href="/search/physics?searchtype=author&query=Checchia%2C+C">C. Checchia</a>, <a href="/search/physics?searchtype=author&query=D%27Alessandro%2C+R">R. D'Alessandro</a>, <a href="/search/physics?searchtype=author&query=Detti%2C+S">S. Detti</a>, <a href="/search/physics?searchtype=author&query=Duranti%2C+M">M. Duranti</a>, <a href="/search/physics?searchtype=author&query=Finetti%2C+N">N. Finetti</a>, <a href="/search/physics?searchtype=author&query=Formato%2C+V">V. Formato</a>, <a href="/search/physics?searchtype=author&query=Ionica%2C+M">M. Ionica</a>, <a href="/search/physics?searchtype=author&query=Maestro%2C+P">P. Maestro</a>, <a href="/search/physics?searchtype=author&query=Maletta%2C+F">F. Maletta</a>, <a href="/search/physics?searchtype=author&query=Marrocchesi%2C+P+S">P. S. Marrocchesi</a>, <a href="/search/physics?searchtype=author&query=Mori%2C+N">N. Mori</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="2008.01390v2-abstract-short" style="display: inline;"> A multi-messenger, space-based cosmic ray detector for gamma rays and charged particles poses several design challenges due to the different instrumental requirements for the two kind of particles. Gamma-ray detection requires layers of high Z materials for photon conversion and a tracking device with a long lever arm to achieve the necessary angular resolution to separate point sources; on the co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.01390v2-abstract-full').style.display = 'inline'; document.getElementById('2008.01390v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.01390v2-abstract-full" style="display: none;"> A multi-messenger, space-based cosmic ray detector for gamma rays and charged particles poses several design challenges due to the different instrumental requirements for the two kind of particles. Gamma-ray detection requires layers of high Z materials for photon conversion and a tracking device with a long lever arm to achieve the necessary angular resolution to separate point sources; on the contrary, charge measurements for atomic nuclei requires a thin detector in order to avoid unwanted fragmentation, and a shallow instrument so to maximize the geometric factor. In this paper, a novel tracking approach for gamma rays which tries to reconcile these two conflicting requirements is presented. The proposal is based on the Tracker-In-Calorimeter (TIC) design that relies on a highly-segmented calorimeter to track the incident gamma ray by sampling the lateral development of the electromagnetic shower at different depths. The effectiveness of this approach has been studied with Monte Carlo simulations and has been validated with test beam data of a detector prototype. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.01390v2-abstract-full').style.display = 'none'; document.getElementById('2008.01390v2-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">17 pages, 8 figures, 2 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 15 P09034 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1806.10948">arXiv:1806.10948</a> <span> [<a href="https://arxiv.org/pdf/1806.10948">pdf</a>, <a href="https://arxiv.org/ps/1806.10948">ps</a>, <a href="https://arxiv.org/format/1806.10948">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/10.3847/1538-4357/aacf89">10.3847/1538-4357/aacf89 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Lithium and Beryllium isotopes with the PAMELA experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Menn%2C+W">W. Menn</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Simon%2C+M">M. Simon</a>, <a href="/search/physics?searchtype=author&query=Vasilyev%2C+G">G. Vasilyev</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=De+Simone%2C+N">N. De Simone</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Formato%2C+V">V. Formato</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Karelin%2C+A+V">A. V. Karelin</a> , et al. (34 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="1806.10948v1-abstract-short" style="display: inline;"> The cosmic-ray lithium and beryllium ($^{6}$Li, $^{7}$Li, $^{7}$Be, $^{9}$Be, $^{10}$Be) isotopic composition has been measured with the satellite-borne experiment PAMELA, which was launched into low-Earth orbit on-board the Resurs-DK1 satellite on June 15th 2006. The rare lithium and beryllium isotopes in cosmic rays are believed to originate mainly from the interaction of high energy carbon, nit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.10948v1-abstract-full').style.display = 'inline'; document.getElementById('1806.10948v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.10948v1-abstract-full" style="display: none;"> The cosmic-ray lithium and beryllium ($^{6}$Li, $^{7}$Li, $^{7}$Be, $^{9}$Be, $^{10}$Be) isotopic composition has been measured with the satellite-borne experiment PAMELA, which was launched into low-Earth orbit on-board the Resurs-DK1 satellite on June 15th 2006. The rare lithium and beryllium isotopes in cosmic rays are believed to originate mainly from the interaction of high energy carbon, nitrogen and oxygen nuclei with the interstellar medium (ISM), but also on "tertiary" interactions in the ISM (i.e. produced by further fragmentation of secondary beryllium and boron). In this paper the isotopic ratios $^{7}$Li/$^{6}$Li and $^{7}$Be/($^{9}$Be + $^{10}$Be) measured between 150 and 1100 MeV/n using two different detector systems from July 2006 to September 2014 will be presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.10948v1-abstract-full').style.display = 'none'; document.getElementById('1806.10948v1-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> 27 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 11 figures, accepted for publication in the Astrophysical Journal. arXiv admin note: text overlap with arXiv:1512.06535</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1803.06166">arXiv:1803.06166</a> <span> [<a href="https://arxiv.org/pdf/1803.06166">pdf</a>, <a href="https://arxiv.org/format/1803.06166">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="Space Physics">physics.space-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/10.3847/1538-4357/aaa0c8">10.3847/1538-4357/aaa0c8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evidence of energy and charge sign dependence of the recovery time for the December 2006 Forbush event measured by the PAMELA experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Munini%2C+R">R. Munini</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Christian%2C+E+C">E. C. Christian</a>, <a href="/search/physics?searchtype=author&query=de+Nolfo%2C+G+A">G. A. de Nolfo</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Martucci%2C+M">M. Martucci</a>, <a href="/search/physics?searchtype=author&query=Merge%2C+M">M. Merge</a>, <a href="/search/physics?searchtype=author&query=Richardson%2C+I+G">I. G. Richardson</a>, <a href="/search/physics?searchtype=author&query=Ryan%2C+J+M">J. M. Ryan</a>, <a href="/search/physics?searchtype=author&query=Stochaj%2C+S">S. Stochaj</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a> , et al. (33 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="1803.06166v1-abstract-short" style="display: inline;"> New results on the short-term galactic cosmic ray (GCR) intensity variation (Forbush decrease) in December 2006 measured by the PAMELA instrument are presented. Forbush decreases are sudden suppressions of the GCR intensities which are associated with the passage of interplanetary transients such as shocks and interplanetary coronal mass ejections (ICMEs). Most of the past measurements of this phe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.06166v1-abstract-full').style.display = 'inline'; document.getElementById('1803.06166v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1803.06166v1-abstract-full" style="display: none;"> New results on the short-term galactic cosmic ray (GCR) intensity variation (Forbush decrease) in December 2006 measured by the PAMELA instrument are presented. Forbush decreases are sudden suppressions of the GCR intensities which are associated with the passage of interplanetary transients such as shocks and interplanetary coronal mass ejections (ICMEs). Most of the past measurements of this phenomenon were carried out with ground-based detectors such as neutron monitors or muon telescopes. These techniques allow only the indirect detection of the overall GCR intensity over an integrated energy range. For the first time, thanks to the unique features of the PAMELA magnetic spectrometer, the Forbush decrease commencing on 2006 December 14, following a CME at the Sun on 2006 December 13 was studied in a wide rigidity range (0.4 - 20 GV) and for different species of GCRs detected directly in space. The daily averaged GCR proton intensity was used to investigate the rigidity dependence of the amplitude and the recovery time of the Forbush decrease. Additionally, for the first time, the temporal variations in the helium and electron intensities during a Forbush decrease were studied. Interestingly, the temporal evolutions of the helium and proton intensities during the Forbush decrease were found in good agreement, while the low rigidity electrons (< 2 GV) displayed a faster recovery. This difference in the electron recovery is interpreted as a charge-sign dependence introduced by drift motions experienced by the GCRs during their propagation through the heliosphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1803.06166v1-abstract-full').style.display = 'none'; document.getElementById('1803.06166v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 March, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ, 853, 76, 2018 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1801.07112">arXiv:1801.07112</a> <span> [<a href="https://arxiv.org/pdf/1801.07112">pdf</a>, <a href="https://arxiv.org/format/1801.07112">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> </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/10.3847/2041-8213/aaa9b2">10.3847/2041-8213/aaa9b2 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Proton fluxes measured by the PAMELA experiment from the minimum to the maximum solar activity for the 24th solar cycle </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Martucci%2C+M">M. Martucci</a>, <a href="/search/physics?searchtype=author&query=Munini%2C+R">R. Munini</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Karelin%2C+A+V">A. V. Karelin</a>, <a href="/search/physics?searchtype=author&query=Koldashov%2C+S+V">S. V. Koldashov</a>, <a href="/search/physics?searchtype=author&query=Koldobskiy%2C+S">S. Koldobskiy</a>, <a href="/search/physics?searchtype=author&query=Krutkov%2C+S+Y">S. Y. Krutkov</a>, <a href="/search/physics?searchtype=author&query=Kvashnin%2C+A+N">A. N. Kvashnin</a>, <a href="/search/physics?searchtype=author&query=Leonov%2C+A">A. Leonov</a> , et al. (29 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="1801.07112v2-abstract-short" style="display: inline;"> Precise measurements of the time-dependent intensity of the low energy ($<50$ GeV) galactic cosmic rays are fundamental to test and improve the models which describe their propagation inside the heliosphere. Especially, data spanning different solar activity periods, i.e. from minimum to maximum, are needed to achieve comprehensive understanding of such physical phenomenon. The minimum phase betwe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.07112v2-abstract-full').style.display = 'inline'; document.getElementById('1801.07112v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.07112v2-abstract-full" style="display: none;"> Precise measurements of the time-dependent intensity of the low energy ($<50$ GeV) galactic cosmic rays are fundamental to test and improve the models which describe their propagation inside the heliosphere. Especially, data spanning different solar activity periods, i.e. from minimum to maximum, are needed to achieve comprehensive understanding of such physical phenomenon. The minimum phase between the 23$^{rd}$ and the 24$^{th}$ solar cycles was peculiarly long, extending up to the beginning of 2010 and followed by the maximum phase, reached during early 2014. In this paper, we present proton differential spectra measured from January 2010 to February 2014 by the PAMELA experiment. For the first time the galactic cosmic ray proton intensity was studied over a wide energy range (0.08-50 GeV) by a single apparatus from a minimum to a maximum period of solar activity. The large statistics allowed the time variation to be investigated on a nearly monthly basis. Data were compared and interpreted in the context of a state-of-the-art three-dimensional model describing the galactic cosmic rays propagation through the heliosphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.07112v2-abstract-full').style.display = 'none'; document.getElementById('1801.07112v2-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> 24 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2018. </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">article, 4 figures. Accepted for publication on The Astrophysical Journal Letters (January 2018)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Letters, Volume 854, Number 1 published 2018 February 5 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1705.07027">arXiv:1705.07027</a> <span> [<a href="https://arxiv.org/pdf/1705.07027">pdf</a>, <a href="https://arxiv.org/format/1705.07027">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> </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/10.1088/1748-0221/12/06/C06004">10.1088/1748-0221/12/06/C06004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CaloCube: a novel calorimeter for high-energy cosmic rays in space </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Cattaneo%2C+P+W">P. W. Cattaneo</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Albergo%2C+S">S. Albergo</a>, <a href="/search/physics?searchtype=author&query=Auditore%2C+L">L. Auditore</a>, <a href="/search/physics?searchtype=author&query=Basti%2C+A">A. Basti</a>, <a href="/search/physics?searchtype=author&query=Berti%2C+E">E. Berti</a>, <a href="/search/physics?searchtype=author&query=Bigongiari%2C+G">G. Bigongiari</a>, <a href="/search/physics?searchtype=author&query=Bonechi%2C+L">L. Bonechi</a>, <a href="/search/physics?searchtype=author&query=Bonechi%2C+S">S. Bonechi</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Brogi%2C+P">P. Brogi</a>, <a href="/search/physics?searchtype=author&query=Carotenuto%2C+G">G. Carotenuto</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=%C4%8FAlessandro%2C+R">R. 膹Alessandro</a>, <a href="/search/physics?searchtype=author&query=Detti%2C+S">S. Detti</a>, <a href="/search/physics?searchtype=author&query=Fasoli%2C+M">M. Fasoli</a>, <a href="/search/physics?searchtype=author&query=Finetti%2C+N">N. Finetti</a>, <a href="/search/physics?searchtype=author&query=Italiano%2C+A">A. Italiano</a>, <a href="/search/physics?searchtype=author&query=Lenzi%2C+P">P. Lenzi</a>, <a href="/search/physics?searchtype=author&query=Maestro%2C+P">P. Maestro</a>, <a href="/search/physics?searchtype=author&query=Marrocchesi%2C+P+S">P. S. Marrocchesi</a>, <a href="/search/physics?searchtype=author&query=Mori%2C+N">N. Mori</a>, <a href="/search/physics?searchtype=author&query=Olmi%2C+M">M. Olmi</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="1705.07027v2-abstract-short" style="display: inline;"> In order to extend the direct observation of high-energy cosmic rays up to the PeV region, highly performing calorimeters with large geometrical acceptance and high energy resolution are required. Within the constraint of the total mass of the apparatus, crucial for a space mission, the calorimeters must be optimized with respect to their geometrical acceptance, granularity and absorption depth. C… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.07027v2-abstract-full').style.display = 'inline'; document.getElementById('1705.07027v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1705.07027v2-abstract-full" style="display: none;"> In order to extend the direct observation of high-energy cosmic rays up to the PeV region, highly performing calorimeters with large geometrical acceptance and high energy resolution are required. Within the constraint of the total mass of the apparatus, crucial for a space mission, the calorimeters must be optimized with respect to their geometrical acceptance, granularity and absorption depth. CaloCube is a homogeneous calorimeter with cubic geometry, to maximise the acceptance being sensitive to particles from every direction in space; granularity is obtained by relying on small cubic scintillating crystals as active elements. Different scintillating materials have been studied. The crystal sizes and spacing among them have been optimized with respect to the energy resolution. A prototype, based on CsI(Tl) cubic crystals, has been constructed and tested with particle beams. Some results of tests with different beams at CERN are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1705.07027v2-abstract-full').style.display = 'none'; document.getElementById('1705.07027v2-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 May, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 May, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Seven pages, seven pictures. Proceedings of INSTR17 Novosibirsk</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1607.02870">arXiv:1607.02870</a> <span> [<a href="https://arxiv.org/pdf/1607.02870">pdf</a>, <a href="https://arxiv.org/ps/1607.02870">ps</a>, <a href="https://arxiv.org/format/1607.02870">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> </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.asr.2016.06.042">10.1016/j.asr.2016.06.042 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Geomagnetically trapped, albedo and solar energetic particles: trajectory analysis and flux reconstruction with PAMELA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Christian%2C+E+C">E. C. Christian</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=de+Nolfo%2C+G+A">G. A. de Nolfo</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=De+Simone%2C+N">N. De Simone</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Karelin%2C+A+V">A. V. Karelin</a>, <a href="/search/physics?searchtype=author&query=Koldashov%2C+S+V">S. V. Koldashov</a>, <a href="/search/physics?searchtype=author&query=Koldobskiy%2C+S">S. Koldobskiy</a> , et al. (37 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="1607.02870v1-abstract-short" style="display: inline;"> The PAMELA satellite experiment is providing comprehensive observations of the interplanetary and magnetospheric radiation in the near-Earth environment. Thanks to its identification capabilities and the semi-polar orbit, PAMELA is able to precisely measure the energetic spectra and the angular distributions of the different cosmic-ray populations over a wide latitude region, including geomagnetic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.02870v1-abstract-full').style.display = 'inline'; document.getElementById('1607.02870v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1607.02870v1-abstract-full" style="display: none;"> The PAMELA satellite experiment is providing comprehensive observations of the interplanetary and magnetospheric radiation in the near-Earth environment. Thanks to its identification capabilities and the semi-polar orbit, PAMELA is able to precisely measure the energetic spectra and the angular distributions of the different cosmic-ray populations over a wide latitude region, including geomagnetically trapped and albedo particles. Its observations comprise the solar energetic particle events between solar cycles 23 and 24, and the geomagnetic cutoff variations during magnetospheric storms. PAMELA's measurements are supported by an accurate analysis of particle trajectories in the Earth's magnetosphere based on a realistic geomagnetic field modeling, which allows the classification of particle populations of different origin and the investigation of the asymptotic directions of arrival. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.02870v1-abstract-full').style.display = 'none'; document.getElementById('1607.02870v1-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 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">Accepted for publication in Advances in Space Research, 2016. 21 pages, 7 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/1602.05509">arXiv:1602.05509</a> <span> [<a href="https://arxiv.org/pdf/1602.05509">pdf</a>, <a href="https://arxiv.org/ps/1602.05509">ps</a>, <a href="https://arxiv.org/format/1602.05509">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="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/10.1002/2016SW001364">10.1002/2016SW001364 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> PAMELA's measurements of geomagnetic cutoff variations during the 14 December 2006 storm </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=de+Nolfo%2C+G+A">G. A. de Nolfo</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=De+Simone%2C+N">N. De Simone</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Karelin%2C+A+V">A. V. Karelin</a>, <a href="/search/physics?searchtype=author&query=Koldashov%2C+S+V">S. V. Koldashov</a>, <a href="/search/physics?searchtype=author&query=Koldobskiy%2C+S">S. Koldobskiy</a>, <a href="/search/physics?searchtype=author&query=Krutkov%2C+S+Y">S. Y. Krutkov</a> , et al. (33 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="1602.05509v2-abstract-short" style="display: inline;"> Data from the Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics (PAMELA) satellite experiment were used to measure the geomagnetic cutoff for high-energy (>80 MeV) protons during the 14 December 2006 geomagnetic storm. The variations of the cutoff latitude as a function of rigidity were studied on relatively short timescales, corresponding to spacecraft orbital periods (94 mi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.05509v2-abstract-full').style.display = 'inline'; document.getElementById('1602.05509v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1602.05509v2-abstract-full" style="display: none;"> Data from the Payload for Antimatter Matter Exploration and Light-nuclei Astrophysics (PAMELA) satellite experiment were used to measure the geomagnetic cutoff for high-energy (>80 MeV) protons during the 14 December 2006 geomagnetic storm. The variations of the cutoff latitude as a function of rigidity were studied on relatively short timescales, corresponding to spacecraft orbital periods (94 min). Estimated cutoff values were compared with those obtained by means of a trajectory tracing approach based on a dynamical empirical modeling of the Earth's magnetosphere. We found significant variations in the cutoff latitude, with a maximum suppression of about 7 deg at lowest rigidities during the main phase of the storm. The observed reduction in the geomagnetic shielding and its temporal evolution were related to the changes in the magnetospheric configuration, investigating the role of interplanetary magnetic field, solar wind and geomagnetic parameters. PAMELA's results represent the first direct measurement of geomagnetic cutoffs for protons with kinetic energies in the sub-GeV and GeV region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1602.05509v2-abstract-full').style.display = 'none'; document.getElementById('1602.05509v2-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 March, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">26 pages, 6 figures and 1 table. Accepted for publication in Space Weather</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1601.05407">arXiv:1601.05407</a> <span> [<a href="https://arxiv.org/pdf/1601.05407">pdf</a>, <a href="https://arxiv.org/ps/1601.05407">ps</a>, <a href="https://arxiv.org/format/1601.05407">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Solar energetic particle events: trajectory analysis and flux reconstruction with PAMELA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Bravar%2C+U">U. Bravar</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carbone%2C+R">R. Carbone</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Christian%2C+E+C">E. C. Christian</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=de+Nolfo%2C+G+A">G. A. de Nolfo</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=De+Simone%2C+N">N. De Simone</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Formato%2C+V">V. Formato</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a> , et al. (42 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="1601.05407v1-abstract-short" style="display: inline;"> The PAMELA satellite experiment is providing first direct measurements of Solar Energetic Particles (SEPs) with energies from about 80 MeV to several GeV in near-Earth space, bridging the low energy data by other space-based instruments and the Ground Level Enhancement (GLE) data by the worldwide network of neutron monitors. Its unique observational capabilities include the possibility of measurin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.05407v1-abstract-full').style.display = 'inline'; document.getElementById('1601.05407v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1601.05407v1-abstract-full" style="display: none;"> The PAMELA satellite experiment is providing first direct measurements of Solar Energetic Particles (SEPs) with energies from about 80 MeV to several GeV in near-Earth space, bridging the low energy data by other space-based instruments and the Ground Level Enhancement (GLE) data by the worldwide network of neutron monitors. Its unique observational capabilities include the possibility of measuring the flux angular distribution and thus investigating possible anisotropies. This work reports the analysis methods developed to estimate the SEP energy spectra as a function of the particle pitch-angle with respect to the Interplanetary Magnetic Field (IMF) direction. The crucial ingredient is provided by an accurate simulation of the asymptotic exposition of the PAMELA apparatus, based on a realistic reconstruction of particle trajectories in the Earth's magnetosphere. As case study, the results for the May 17, 2012 event are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.05407v1-abstract-full').style.display = 'none'; document.getElementById('1601.05407v1-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, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">Conference: The 34th International Cosmic Ray Conference (ICRC2015), 30 July - 6 August, 2015, The Hague, The Netherlands, Volume: PoS(ICRC2015)085</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.00543">arXiv:1511.00543</a> <span> [<a href="https://arxiv.org/pdf/1511.00543">pdf</a>, <a href="https://arxiv.org/ps/1511.00543">ps</a>, <a href="https://arxiv.org/format/1511.00543">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> PAMELA's measurements of geomagnetically trapped and albedo protons </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Bravar%2C+U">U. Bravar</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carbone%2C+R">R. Carbone</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Christian%2C+E+C">E. C. Christian</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=de+Nolfo%2C+G+A">G. A. de Nolfo</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=De+Simone%2C+N">N. De Simone</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Formato%2C+V">V. Formato</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a> , et al. (42 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="1511.00543v2-abstract-short" style="display: inline;"> Data from the PAMELA satellite experiment were used to perform a detailed measurement of under-cutoff protons at low Earth orbits. On the basis of a trajectory tracing approach using a realistic description of the magnetosphere, protons were classified into geomagnetically trapped and re-entrant albedo. The former include stably-trapped protons in the South Atlantic Anomaly, which were analyzed in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.00543v2-abstract-full').style.display = 'inline'; document.getElementById('1511.00543v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.00543v2-abstract-full" style="display: none;"> Data from the PAMELA satellite experiment were used to perform a detailed measurement of under-cutoff protons at low Earth orbits. On the basis of a trajectory tracing approach using a realistic description of the magnetosphere, protons were classified into geomagnetically trapped and re-entrant albedo. The former include stably-trapped protons in the South Atlantic Anomaly, which were analyzed in the framework of the adiabatic theory, investigating energy spectra, spatial and angular distributions; results were compared with the predictions of the AP8 and the PSB97 empirical trapped models. The albedo protons were classified into quasi-trapped, concentrating in the magnetic equatorial region, and un-trapped, spreading over all latitudes and including both short-lived (precipitating) and long-lived (pseudo-trapped) components. Features of the penumbra region around the geomagnetic cutoff were investigated as well. PAMELA observations significantly improve the characterization of the high energy proton populations in near Earth orbits. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.00543v2-abstract-full').style.display = 'none'; document.getElementById('1511.00543v2-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 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Conference: The 34th International Cosmic Ray Conference (ICRC2015), 30 July - 6 August, 2015, The Hague, The Netherlands, Volume: PoS(ICRC2015)288</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.00530">arXiv:1511.00530</a> <span> [<a href="https://arxiv.org/pdf/1511.00530">pdf</a>, <a href="https://arxiv.org/ps/1511.00530">ps</a>, <a href="https://arxiv.org/format/1511.00530">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> PAMELA's measurements of geomagnetic cutoff variations during solar energetic particle events </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Bravar%2C+U">U. Bravar</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carbone%2C+R">R. Carbone</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Christian%2C+E+C">E. C. Christian</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=de+Nolfo%2C+G+A">G. A. de Nolfo</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=De+Simone%2C+N">N. De Simone</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Formato%2C+V">V. Formato</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a> , et al. (42 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="1511.00530v1-abstract-short" style="display: inline;"> Data from the PAMELA satellite experiment were used to measure the geomagnetic cutoff for high-energy ($\gtrsim$ 80 MeV) protons during the solar particle events on 2006 December 13 and 14. The variations of the cutoff latitude as a function of rigidity were studied on relatively short timescales, corresponding to single spacecraft orbits (about 94 minutes). Estimated cutoff values were cross-chec… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.00530v1-abstract-full').style.display = 'inline'; document.getElementById('1511.00530v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.00530v1-abstract-full" style="display: none;"> Data from the PAMELA satellite experiment were used to measure the geomagnetic cutoff for high-energy ($\gtrsim$ 80 MeV) protons during the solar particle events on 2006 December 13 and 14. The variations of the cutoff latitude as a function of rigidity were studied on relatively short timescales, corresponding to single spacecraft orbits (about 94 minutes). Estimated cutoff values were cross-checked with those obtained by means of a trajectory tracing approach based on dynamical empirical modeling of the Earth's magnetosphere. We find significant variations in the cutoff latitude, with a maximum suppression of about 6 deg for $\sim$80 MeV protons during the main phase of the storm. The observed reduction in the geomagnetic shielding and its temporal evolution were compared with the changes in the magnetosphere configuration, investigating the role of IMF, solar wind and geomagnetic (Kp, Dst and Sym-H indexes) variables and their correlation with PAMELA cutoff results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.00530v1-abstract-full').style.display = 'none'; document.getElementById('1511.00530v1-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, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Conference: The 34th International Cosmic Ray Conference (ICRC2015), 30 July - 6 August, 2015, The Hague, The Netherlands, Volume: PoS(ICRC2015)287</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1504.06253">arXiv:1504.06253</a> <span> [<a href="https://arxiv.org/pdf/1504.06253">pdf</a>, <a href="https://arxiv.org/ps/1504.06253">ps</a>, <a href="https://arxiv.org/format/1504.06253">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="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> Re-Entrant Albedo Proton Fluxes Measured by the PAMELA Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=De+Simone%2C+N">N. De Simone</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Formato%2C+V">V. Formato</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Karelin%2C+A+V">A. V. Karelin</a>, <a href="/search/physics?searchtype=author&query=Koldashov%2C+S+V">S. V. Koldashov</a>, <a href="/search/physics?searchtype=author&query=Koldobskiy%2C+S">S. Koldobskiy</a>, <a href="/search/physics?searchtype=author&query=Krutkov%2C+S+Y">S. Y. Krutkov</a> , et al. (34 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="1504.06253v1-abstract-short" style="display: inline;"> We present a precise measurement of downward-going albedo proton fluxes for kinetic energy above $\sim$ 70 MeV performed by the PAMELA experiment at an altitude between 350 and 610 km. On the basis of a trajectory tracing simulation, the analyzed protons were classified into quasi-trapped, concentrating in the magnetic equatorial region, and un-trapped spreading over all latitudes, including both… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.06253v1-abstract-full').style.display = 'inline'; document.getElementById('1504.06253v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1504.06253v1-abstract-full" style="display: none;"> We present a precise measurement of downward-going albedo proton fluxes for kinetic energy above $\sim$ 70 MeV performed by the PAMELA experiment at an altitude between 350 and 610 km. On the basis of a trajectory tracing simulation, the analyzed protons were classified into quasi-trapped, concentrating in the magnetic equatorial region, and un-trapped spreading over all latitudes, including both short-lived (precipitating) and long-lived (pseudo-trapped) components. In addition, features of the penumbra region around the geomagnetic cutoff were investigated in detail. PAMELA results significantly improve the characterization of the high energy albedo proton populations at low Earth orbits. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.06253v1-abstract-full').style.display = 'none'; document.getElementById('1504.06253v1-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 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">28 pages, 8 figures. Accepted for publication in Journal of Geophysical Research - Space Physics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1503.06657">arXiv:1503.06657</a> <span> [<a href="https://arxiv.org/pdf/1503.06657">pdf</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="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.asr.2015.06.040">10.1016/j.asr.2015.06.040 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A separation of electrons and protons in the GAMMA-400 gamma-ray telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Leonov%2C+A+A">A. A. Leonov</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Topchiev%2C+N+P">N. P. Topchiev</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Aptekar%2C+R+L">R. L. Aptekar</a>, <a href="/search/physics?searchtype=author&query=Arkhangelskaja%2C+I+V">I. V. Arkhangelskaja</a>, <a href="/search/physics?searchtype=author&query=Arkhangelskiy%2C+A+I">A. I. Arkhangelskiy</a>, <a href="/search/physics?searchtype=author&query=Bergstrom%2C+L">L. Bergstrom</a>, <a href="/search/physics?searchtype=author&query=Berti%2C+E">E. Berti</a>, <a href="/search/physics?searchtype=author&query=Bigongiari%2C+G">G. Bigongiari</a>, <a href="/search/physics?searchtype=author&query=Bobkov%2C+S+G">S. G. Bobkov</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bonechi%2C+S">S. Bonechi</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Cattaneo%2C+P+W">P. W. Cattaneo</a>, <a href="/search/physics?searchtype=author&query=Cumani%2C+P">P. Cumani</a>, <a href="/search/physics?searchtype=author&query=Dedenko%2C+G+L">G. L. Dedenko</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=Dogiel%2C+V+A">V. A. Dogiel</a>, <a href="/search/physics?searchtype=author&query=Gorbunov%2C+M+S">M. S. Gorbunov</a>, <a href="/search/physics?searchtype=author&query=Gusakov%2C+Y+V">Yu. V. Gusakov</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="1503.06657v1-abstract-short" style="display: inline;"> The GAMMA-400 gamma-ray telescope is intended to measure the fluxes of gamma rays and cosmic-ray electrons and positrons in the energy range from 100 MeV to several TeV. Such measurements concern with the following scientific goals: search for signatures of dark matter, investigation of gamma-ray point and extended sources, studies of the energy spectra of Galactic and extragalactic diffuse emissi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.06657v1-abstract-full').style.display = 'inline'; document.getElementById('1503.06657v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.06657v1-abstract-full" style="display: none;"> The GAMMA-400 gamma-ray telescope is intended to measure the fluxes of gamma rays and cosmic-ray electrons and positrons in the energy range from 100 MeV to several TeV. Such measurements concern with the following scientific goals: search for signatures of dark matter, investigation of gamma-ray point and extended sources, studies of the energy spectra of Galactic and extragalactic diffuse emission, studies of gamma-ray bursts and gamma-ray emission from the active Sun, as well as high-precision measurements of spectra of high-energy electrons and positrons, protons, and nuclei up to the knee. The main components of cosmic rays are protons and helium nuclei, whereas the part of lepton component in the total flux is ~10E-3 for high energies. In present paper, the capability of the GAMMA-400 gamma-ray telescope to distinguish electrons and positrons from protons in cosmic rays is investigated. The individual contribution to the proton rejection is studied for each detector system of the GAMMA-400 gamma-ray telescope. Using combined information from all detector systems allow us to provide the proton rejection from electrons with a factor of ~4x10E5 for vertical incident particles and ~3x10E5 for particles with initial inclination of 30 degrees. The calculations were performed for the electron energy range from 50 GeV to 1 TeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.06657v1-abstract-full').style.display = 'none'; document.getElementById('1503.06657v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 March, 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">19 pages, 10 figures, submitted to Advances and Space Research</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1412.4239">arXiv:1412.4239</a> <span> [<a href="https://arxiv.org/pdf/1412.4239">pdf</a>, <a href="https://arxiv.org/format/1412.4239">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 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> </div> </div> <p class="title is-5 mathjax"> The GAMMA-400 space observatory: status and perspectives </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Topchiev%2C+N+P">N. P. Topchiev</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Aptekar%2C+R+L">R. L. Aptekar</a>, <a href="/search/physics?searchtype=author&query=Arkhangelskaja%2C+I+V">I. V. Arkhangelskaja</a>, <a href="/search/physics?searchtype=author&query=Arkhangelskiy%2C+A+I">A. I. Arkhangelskiy</a>, <a href="/search/physics?searchtype=author&query=Bergstrom%2C+L">L. Bergstrom</a>, <a href="/search/physics?searchtype=author&query=Berti%2C+E">E. Berti</a>, <a href="/search/physics?searchtype=author&query=Bigongiari%2C+G">G. Bigongiari</a>, <a href="/search/physics?searchtype=author&query=Bobkov%2C+S+G">S. G. Bobkov</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bonechi%2C+S">S. Bonechi</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Boyarchuk%2C+K+A">K. A. Boyarchuk</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Cattaneo%2C+P+W">P. W. Cattaneo</a>, <a href="/search/physics?searchtype=author&query=Cumani%2C+P">P. Cumani</a>, <a href="/search/physics?searchtype=author&query=Dedenko%2C+G+L">G. L. Dedenko</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=Dogiel%2C+V+A">V. A. Dogiel</a>, <a href="/search/physics?searchtype=author&query=Gorbunov%2C+M+S">M. S. Gorbunov</a>, <a href="/search/physics?searchtype=author&query=Gusakov%2C+Y+V">Yu. V. Gusakov</a> , et al. (42 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="1412.4239v1-abstract-short" style="display: inline;"> The present design of the new space observatory GAMMA-400 is presented in this paper. The instrument has been designed for the optimal detection of gamma rays in a broad energy range (from ~100 MeV up to 3 TeV), with excellent angular and energy resolution. The observatory will also allow precise and high statistic studies of the electron component in the cosmic rays up to the multi TeV region, as… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.4239v1-abstract-full').style.display = 'inline'; document.getElementById('1412.4239v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1412.4239v1-abstract-full" style="display: none;"> The present design of the new space observatory GAMMA-400 is presented in this paper. The instrument has been designed for the optimal detection of gamma rays in a broad energy range (from ~100 MeV up to 3 TeV), with excellent angular and energy resolution. The observatory will also allow precise and high statistic studies of the electron component in the cosmic rays up to the multi TeV region, as well as protons and nuclei spectra up to the knee region. The GAMMA-400 observatory will allow to address a broad range of science topics, like search for signatures of dark matter, studies of Galactic and extragalactic gamma-ray sources, Galactic and extragalactic diffuse emission, gamma-ray bursts and charged cosmic rays acceleration and diffusion mechanism up to the knee. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.4239v1-abstract-full').style.display = 'none'; document.getElementById('1412.4239v1-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 December, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2014. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1412.1765">arXiv:1412.1765</a> <span> [<a href="https://arxiv.org/pdf/1412.1765">pdf</a>, <a href="https://arxiv.org/ps/1412.1765">ps</a>, <a href="https://arxiv.org/format/1412.1765">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-ph</span> </div> </div> <p class="title is-5 mathjax"> Back-Tracing and Flux Reconstruction for Solar Events with PAMELA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Bravar%2C+U">U. Bravar</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carbone%2C+R">R. Carbone</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Christian%2C+E+C">E. C. Christian</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=de+Nolfo%2C+G+A">G. A. de Nolfo</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=De+Simone%2C+N">N. De Simone</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Formato%2C+V">V. Formato</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a> , et al. (42 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="1412.1765v5-abstract-short" style="display: inline;"> The PAMELA satellite-borne experiment is providing first direct measurements of Solar Energetic Particles (SEPs) with energies from $\sim$80 MeV to several GeV in near-Earth space. Its unique observational capabilities include the possibility of measuring the flux angular distribution and thus investigating possible anisotropies related to SEP events. This paper focuses on the analysis methods dev… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.1765v5-abstract-full').style.display = 'inline'; document.getElementById('1412.1765v5-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1412.1765v5-abstract-full" style="display: none;"> The PAMELA satellite-borne experiment is providing first direct measurements of Solar Energetic Particles (SEPs) with energies from $\sim$80 MeV to several GeV in near-Earth space. Its unique observational capabilities include the possibility of measuring the flux angular distribution and thus investigating possible anisotropies related to SEP events. This paper focuses on the analysis methods developed to estimate SEP energy spectra as a function of the particle pitch angle with respect to the Interplanetary Magnetic Field (IMF). The crucial ingredient is provided by an accurate simulation of the asymptotic exposition of the PAMELA apparatus, based on a realistic reconstruction of particle trajectories in the Earth's magnetosphere. As case study, the results of the calculation for the May 17, 2012 event are reported. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.1765v5-abstract-full').style.display = 'none'; document.getElementById('1412.1765v5-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, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 December, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">25 pages, 9 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/1412.1258">arXiv:1412.1258</a> <span> [<a href="https://arxiv.org/pdf/1412.1258">pdf</a>, <a href="https://arxiv.org/ps/1412.1258">ps</a>, <a href="https://arxiv.org/format/1412.1258">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-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/10.1088/2041-8205/799/1/L4">10.1088/2041-8205/799/1/L4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Trapped proton fluxes at low Earth orbits measured by the PAMELA experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G+C">G. C. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Bazilevskaya%2C+G+A">G. A. Bazilevskaya</a>, <a href="/search/physics?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/physics?searchtype=author&query=Boezio%2C+M">M. Boezio</a>, <a href="/search/physics?searchtype=author&query=Bogomolov%2C+E+A">E. A. Bogomolov</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bonvicini%2C+V">V. Bonvicini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+A">A. Bruno</a>, <a href="/search/physics?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/physics?searchtype=author&query=Campana%2C+D">D. Campana</a>, <a href="/search/physics?searchtype=author&query=Carbone%2C+R">R. Carbone</a>, <a href="/search/physics?searchtype=author&query=Carlson%2C+P">P. Carlson</a>, <a href="/search/physics?searchtype=author&query=Casolino%2C+M">M. Casolino</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=Danilchenko%2C+I+A">I. A. Danilchenko</a>, <a href="/search/physics?searchtype=author&query=De+Donato%2C+C">C. De Donato</a>, <a href="/search/physics?searchtype=author&query=De+Santis%2C+C">C. De Santis</a>, <a href="/search/physics?searchtype=author&query=De+Simone%2C+N">N. De Simone</a>, <a href="/search/physics?searchtype=author&query=Di+Felice%2C+V">V. Di Felice</a>, <a href="/search/physics?searchtype=author&query=Formato%2C+V">V. Formato</a>, <a href="/search/physics?searchtype=author&query=Galper%2C+A+M">A. M. Galper</a>, <a href="/search/physics?searchtype=author&query=Karelin%2C+A+V">A. V. Karelin</a>, <a href="/search/physics?searchtype=author&query=Koldashov%2C+S+V">S. V. Koldashov</a> , et al. (37 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="1412.1258v2-abstract-short" style="display: inline;"> We report an accurate measurement of the geomagnetically trapped proton fluxes for kinetic energy above > 70 MeV performed by the PAMELA mission at low Earth orbits (350-610 km). Data were analyzed in the frame of the adiabatic theory of charged particle motion in the geomagnetic field. Flux properties were investigated in detail, providing a full characterization of the particle radiation in the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.1258v2-abstract-full').style.display = 'inline'; document.getElementById('1412.1258v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1412.1258v2-abstract-full" style="display: none;"> We report an accurate measurement of the geomagnetically trapped proton fluxes for kinetic energy above > 70 MeV performed by the PAMELA mission at low Earth orbits (350-610 km). Data were analyzed in the frame of the adiabatic theory of charged particle motion in the geomagnetic field. Flux properties were investigated in detail, providing a full characterization of the particle radiation in the South Atlantic Anomaly region, including locations, energy spectra and pitch angle distributions. PAMELA results significantly improve the description of the Earth's radiation environment at low altitudes placing important constraints on the trapping and interaction processes, and can be used to validate current trapped particle radiation models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.1258v2-abstract-full').style.display = 'none'; document.getElementById('1412.1258v2-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 January, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 December, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">22 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 799 L4, 2015 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1008.2392">arXiv:1008.2392</a> <span> [<a href="https://arxiv.org/pdf/1008.2392">pdf</a>, <a href="https://arxiv.org/format/1008.2392">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> </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/10.1088/1742-6596/293/1/012039">10.1088/1742-6596/293/1/012039 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NEUCAL, an innovative neutron detector for e/h discrimination: testbeam results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Sguazzoni%2C+G">G. Sguazzoni</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=Bonechi%2C+L">L. Bonechi</a>, <a href="/search/physics?searchtype=author&query=Bongi%2C+M">M. Bongi</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Calamai%2C+M">M. Calamai</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</a>, <a href="/search/physics?searchtype=author&query=D%27Alessandro%2C+R">R. D'Alessandro</a>, <a href="/search/physics?searchtype=author&query=Grandi%2C+M">M. Grandi</a>, <a href="/search/physics?searchtype=author&query=Papini%2C+P">P. Papini</a>, <a href="/search/physics?searchtype=author&query=Ricciarini%2C+S">S. Ricciarini</a>, <a href="/search/physics?searchtype=author&query=Sona%2C+P">P. Sona</a>, <a href="/search/physics?searchtype=author&query=Sorichetti%2C+G">G. Sorichetti</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="1008.2392v1-abstract-short" style="display: inline;"> An excellent hadron to electron discrimination is a crucial aspect of calorimeter-based experiments in astroparticle physics. Standard discrimination techniques require full shower development and fine granularity but in space detectors severe limitations exist due to constraints on dimensions, weight and power consumption. A possible approach is to exploit the different neutron yield of electroma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1008.2392v1-abstract-full').style.display = 'inline'; document.getElementById('1008.2392v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1008.2392v1-abstract-full" style="display: none;"> An excellent hadron to electron discrimination is a crucial aspect of calorimeter-based experiments in astroparticle physics. Standard discrimination techniques require full shower development and fine granularity but in space detectors severe limitations exist due to constraints on dimensions, weight and power consumption. A possible approach is to exploit the different neutron yield of electromagnetic and hadronic showers. NEUCAL is a light and compact innovative neutron detector, to be used as an auxiliary complement of electromagnetic calorimeters. This new approach to neutron counting relies on scintillation detectors which are sensitive to the moderation phase of the neutron component. The NEUCAL prototype has been placed after a conventional calorimeter and tested with high energy beams of pions and positrons. The comparison of experimental data with a detailed Geant4 simulation and the encouraging results obtained are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1008.2392v1-abstract-full').style.display = 'none'; document.getElementById('1008.2392v1-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 August, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6 pages, 7 figures, presented at CALOR 2010, XIV International Conference on Calorimetry in High Energy Physics, 10-14 May 2010, Beijing (China)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J.Phys.Conf.Ser.293:012039,2011 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1008.1886">arXiv:1008.1886</a> <span> [<a href="https://arxiv.org/pdf/1008.1886">pdf</a>, <a href="https://arxiv.org/ps/1008.1886">ps</a>, <a href="https://arxiv.org/format/1008.1886">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> </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/10.1142/9789814307529_0120">10.1142/9789814307529_0120 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> NEUCAL: a prototype detector for electron/hadron discrimination through neutron measurement </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bonechi%2C+L">L. Bonechi</a>, <a href="/search/physics?searchtype=author&query=Adriani%2C+O">O. Adriani</a>, <a href="/search/physics?searchtype=author&query=D%27Alessandro%2C+R">R. D'Alessandro</a>, <a href="/search/physics?searchtype=author&query=Sona%2C+P">P. Sona</a>, <a href="/search/physics?searchtype=author&query=Sorichetti%2C+G">G. Sorichetti</a>, <a href="/search/physics?searchtype=author&query=Spillantini%2C+P">P. Spillantini</a>, <a href="/search/physics?searchtype=author&query=Bottai%2C+S">S. Bottai</a>, <a href="/search/physics?searchtype=author&query=Grandi%2C+M">M. Grandi</a>, <a href="/search/physics?searchtype=author&query=Papini%2C+P">P. Papini</a>, <a href="/search/physics?searchtype=author&query=Ricciarini%2C+S">S. Ricciarini</a>, <a href="/search/physics?searchtype=author&query=Sguazzoni%2C+G">G. Sguazzoni</a>, <a href="/search/physics?searchtype=author&query=Vannuccini%2C+E">E. Vannuccini</a>, <a href="/search/physics?searchtype=author&query=Viciani%2C+A">A. Viciani</a>, <a href="/search/physics?searchtype=author&query=Castellini%2C+G">G. Castellini</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="1008.1886v1-abstract-short" style="display: inline;"> NEUCAL is a neutron detector which is currently under study to be used as a sub-detector complementing electromagnetic (e.m.) calorimeters for electron/hadron discrimination in cosmic rays at high energy. Its aim is to reveal the different yield of neutron production in e.m. and hadronic showers, not only by counting signals due to their absorption in some sensible detector after passive moderatio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1008.1886v1-abstract-full').style.display = 'inline'; document.getElementById('1008.1886v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1008.1886v1-abstract-full" style="display: none;"> NEUCAL is a neutron detector which is currently under study to be used as a sub-detector complementing electromagnetic (e.m.) calorimeters for electron/hadron discrimination in cosmic rays at high energy. Its aim is to reveal the different yield of neutron production in e.m. and hadronic showers, not only by counting signals due to their absorption in some sensible detector after passive moderation, but also looking for signals produced during the moderation phase. The basic idea and a test of a prototype detector are discussed in this paper. A first preliminary comparison of experimental data with simulation is also shown. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1008.1886v1-abstract-full').style.display = 'none'; document.getElementById('1008.1886v1-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, 2010; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2010. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 6 figures, "11th ICATPP Conference on Astroparticle, Particle, Space Physics, Detectors and Medical Physics Applications"</span> </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