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<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/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/1511.00556">arXiv:1511.00556</a> <span> [<a href="https://arxiv.org/pdf/1511.00556">pdf</a>, <a href="https://arxiv.org/format/1511.00556">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/10.1088/1748-0221/11/03/P03001">10.1088/1748-0221/11/03/P03001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Pion contamination in the MICE muon beam </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adams%2C+D">D. Adams</a>, <a href="/search/physics?searchtype=author&query=Alekou%2C+A">A. Alekou</a>, <a href="/search/physics?searchtype=author&query=Apollonio%2C+M">M. Apollonio</a>, <a href="/search/physics?searchtype=author&query=Asfandiyarov%2C+R">R. Asfandiyarov</a>, <a href="/search/physics?searchtype=author&query=Barber%2C+G">G. Barber</a>, <a href="/search/physics?searchtype=author&query=Barclay%2C+P">P. Barclay</a>, <a href="/search/physics?searchtype=author&query=de+Bari%2C+A">A. de Bari</a>, <a href="/search/physics?searchtype=author&query=Bayes%2C+R">R. Bayes</a>, <a href="/search/physics?searchtype=author&query=Bayliss%2C+V">V. Bayliss</a>, <a href="/search/physics?searchtype=author&query=Bertoni%2C+R">R. Bertoni</a>, <a href="/search/physics?searchtype=author&query=Blackmore%2C+V+J">V. J. Blackmore</a>, <a href="/search/physics?searchtype=author&query=Blondel%2C+A">A. Blondel</a>, <a href="/search/physics?searchtype=author&query=Blot%2C+S">S. Blot</a>, <a href="/search/physics?searchtype=author&query=Bogomilov%2C+M">M. Bogomilov</a>, <a href="/search/physics?searchtype=author&query=Bonesini%2C+M">M. Bonesini</a>, <a href="/search/physics?searchtype=author&query=Booth%2C+C+N">C. N. Booth</a>, <a href="/search/physics?searchtype=author&query=Bowring%2C+D">D. Bowring</a>, <a href="/search/physics?searchtype=author&query=Boyd%2C+S">S. Boyd</a>, <a href="/search/physics?searchtype=author&query=Bradshaw%2C+T+W">T. W. Bradshaw</a>, <a href="/search/physics?searchtype=author&query=Bravar%2C+U">U. Bravar</a>, <a href="/search/physics?searchtype=author&query=Bross%2C+A+D">A. D. Bross</a>, <a href="/search/physics?searchtype=author&query=Capponi%2C+M">M. Capponi</a>, <a href="/search/physics?searchtype=author&query=Carlisle%2C+T">T. Carlisle</a>, <a href="/search/physics?searchtype=author&query=Cecchet%2C+G">G. Cecchet</a>, <a href="/search/physics?searchtype=author&query=Charnley%2C+C">C. Charnley</a> , et al. (120 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="1511.00556v3-abstract-short" style="display: inline;"> The international Muon Ionization Cooling Experiment (MICE) will perform a systematic investigation of ionization cooling with muon beams of momentum between 140 and 240\,MeV/c at the Rutherford Appleton Laboratory ISIS facility. The measurement of ionization cooling in MICE relies on the selection of a pure sample of muons that traverse the experiment. To make this selection, the MICE Muon Beam i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.00556v3-abstract-full').style.display = 'inline'; document.getElementById('1511.00556v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.00556v3-abstract-full" style="display: none;"> The international Muon Ionization Cooling Experiment (MICE) will perform a systematic investigation of ionization cooling with muon beams of momentum between 140 and 240\,MeV/c at the Rutherford Appleton Laboratory ISIS facility. The measurement of ionization cooling in MICE relies on the selection of a pure sample of muons that traverse the experiment. To make this selection, the MICE Muon Beam is designed to deliver a beam of muons with less than $\sim$1\% contamination. To make the final muon selection, MICE employs a particle-identification (PID) system upstream and downstream of the cooling cell. The PID system includes time-of-flight hodoscopes, threshold-Cherenkov counters and calorimetry. The upper limit for the pion contamination measured in this paper is $f_蟺< 1.4\%$ at 90\% C.L., including systematic uncertainties. Therefore, the MICE Muon Beam is able to meet the stringent pion-contamination requirements of the study of ionization cooling. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.00556v3-abstract-full').style.display = 'none'; document.getElementById('1511.00556v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 February, 2016; <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">16 pages, 7 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> RAL-P-2015-009 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 11 (2016) 03, P03002 </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/1510.08306">arXiv:1510.08306</a> <span> [<a href="https://arxiv.org/pdf/1510.08306">pdf</a>, <a href="https://arxiv.org/format/1510.08306">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/10.1088/1748-0221/10/12/P12012">10.1088/1748-0221/10/12/P12012 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Electron-Muon Ranger: performance in the MICE Muon Beam </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adams%2C+D">D. Adams</a>, <a href="/search/physics?searchtype=author&query=Alekou%2C+A">A. Alekou</a>, <a href="/search/physics?searchtype=author&query=Apollonio%2C+M">M. Apollonio</a>, <a href="/search/physics?searchtype=author&query=Asfandiyarov%2C+R">R. Asfandiyarov</a>, <a href="/search/physics?searchtype=author&query=Barber%2C+G">G. Barber</a>, <a href="/search/physics?searchtype=author&query=Barclay%2C+P">P. Barclay</a>, <a href="/search/physics?searchtype=author&query=de+Bari%2C+A">A. de Bari</a>, <a href="/search/physics?searchtype=author&query=Bayes%2C+R">R. Bayes</a>, <a href="/search/physics?searchtype=author&query=Bayliss%2C+V">V. Bayliss</a>, <a href="/search/physics?searchtype=author&query=Bene%2C+P">P. Bene</a>, <a href="/search/physics?searchtype=author&query=Bertoni%2C+R">R. Bertoni</a>, <a href="/search/physics?searchtype=author&query=Blackmore%2C+V+J">V. J. Blackmore</a>, <a href="/search/physics?searchtype=author&query=Blondel%2C+A">A. Blondel</a>, <a href="/search/physics?searchtype=author&query=Blot%2C+S">S. Blot</a>, <a href="/search/physics?searchtype=author&query=Bogomilov%2C+M">M. Bogomilov</a>, <a href="/search/physics?searchtype=author&query=Bonesini%2C+M">M. Bonesini</a>, <a href="/search/physics?searchtype=author&query=Booth%2C+C+N">C. N. Booth</a>, <a href="/search/physics?searchtype=author&query=Bowring%2C+D">D. Bowring</a>, <a href="/search/physics?searchtype=author&query=Boyd%2C+S">S. Boyd</a>, <a href="/search/physics?searchtype=author&query=Bradshaw%2C+T+W">T. W. Bradshaw</a>, <a href="/search/physics?searchtype=author&query=Bravar%2C+U">U. Bravar</a>, <a href="/search/physics?searchtype=author&query=Bross%2C+A+D">A. D. Bross</a>, <a href="/search/physics?searchtype=author&query=Cadoux%2C+F">F. Cadoux</a>, <a href="/search/physics?searchtype=author&query=Capponi%2C+M">M. Capponi</a>, <a href="/search/physics?searchtype=author&query=Carlisle%2C+T">T. Carlisle</a> , et al. (129 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="1510.08306v2-abstract-short" style="display: inline;"> The Muon Ionization Cooling Experiment (MICE) will perform a detailed study of ionization cooling to evaluate the feasibility of the technique. To carry out this program, MICE requires an efficient particle-identification (PID) system to identify muons. The Electron-Muon Ranger (EMR) is a fully-active tracking-calorimeter that forms part of the PID system and tags muons that traverse the cooling c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.08306v2-abstract-full').style.display = 'inline'; document.getElementById('1510.08306v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1510.08306v2-abstract-full" style="display: none;"> The Muon Ionization Cooling Experiment (MICE) will perform a detailed study of ionization cooling to evaluate the feasibility of the technique. To carry out this program, MICE requires an efficient particle-identification (PID) system to identify muons. The Electron-Muon Ranger (EMR) is a fully-active tracking-calorimeter that forms part of the PID system and tags muons that traverse the cooling channel without decaying. The detector is capable of identifying electrons with an efficiency of 98.6%, providing a purity for the MICE beam that exceeds 99.8%. The EMR also proved to be a powerful tool for the reconstruction of muon momenta in the range 100-280 MeV/$c$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.08306v2-abstract-full').style.display = 'none'; document.getElementById('1510.08306v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 October, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 19 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> RAL-P-2015-008 </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/1306.1509">arXiv:1306.1509</a> <span> [<a href="https://arxiv.org/pdf/1306.1509">pdf</a>, <a href="https://arxiv.org/ps/1306.1509">ps</a>, <a href="https://arxiv.org/format/1306.1509">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Accelerator Physics">physics.acc-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/10.1140/epjc/s10052-013-2582-8">10.1140/epjc/s10052-013-2582-8 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterisation of the muon beams for the Muon Ionisation Cooling Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=The+MICE+Collaboration"> The MICE Collaboration</a>, <a href="/search/physics?searchtype=author&query=Adams%2C+D">D. Adams</a>, <a href="/search/physics?searchtype=author&query=Adey%2C+D">D. Adey</a>, <a href="/search/physics?searchtype=author&query=Alekou%2C+A">A. Alekou</a>, <a href="/search/physics?searchtype=author&query=Apollonio%2C+M">M. Apollonio</a>, <a href="/search/physics?searchtype=author&query=Asfandiyarov%2C+R">R. Asfandiyarov</a>, <a href="/search/physics?searchtype=author&query=Back%2C+J">J. Back</a>, <a href="/search/physics?searchtype=author&query=Barber%2C+G">G. Barber</a>, <a href="/search/physics?searchtype=author&query=Barclay%2C+P">P. Barclay</a>, <a href="/search/physics?searchtype=author&query=de+Bari%2C+A">A. de Bari</a>, <a href="/search/physics?searchtype=author&query=Bayes%2C+R">R. Bayes</a>, <a href="/search/physics?searchtype=author&query=Bayliss%2C+V">V. Bayliss</a>, <a href="/search/physics?searchtype=author&query=Bertoni%2C+R">R. Bertoni</a>, <a href="/search/physics?searchtype=author&query=Blackmore%2C+V+J">V. J. Blackmore</a>, <a href="/search/physics?searchtype=author&query=Blondel%2C+A">A. Blondel</a>, <a href="/search/physics?searchtype=author&query=Blot%2C+S">S. Blot</a>, <a href="/search/physics?searchtype=author&query=Bogomilov%2C+M">M. Bogomilov</a>, <a href="/search/physics?searchtype=author&query=Bonesini%2C+M">M. Bonesini</a>, <a href="/search/physics?searchtype=author&query=Booth%2C+C+N">C. N. Booth</a>, <a href="/search/physics?searchtype=author&query=Bowring%2C+D">D. Bowring</a>, <a href="/search/physics?searchtype=author&query=Boyd%2C+S">S. Boyd</a>, <a href="/search/physics?searchtype=author&query=Bradshaw%2C+T+W">T. W. Bradshaw</a>, <a href="/search/physics?searchtype=author&query=Bravar%2C+U">U. Bravar</a>, <a href="/search/physics?searchtype=author&query=Bross%2C+A+D">A. D. Bross</a>, <a href="/search/physics?searchtype=author&query=Capponi%2C+M">M. Capponi</a> , et al. (119 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="1306.1509v2-abstract-short" style="display: inline;"> A novel single-particle technique to measure emittance has been developed and used to characterise seventeen different muon beams for the Muon Ionisation Cooling Experiment (MICE). The muon beams, whose mean momenta vary from 171 to 281 MeV/c, have emittances of approximately 1.5--2.3 蟺mm-rad horizontally and 0.6--1.0 蟺mm-rad vertically, a horizontal dispersion of 90--190 mm and momentum spreads o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1306.1509v2-abstract-full').style.display = 'inline'; document.getElementById('1306.1509v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1306.1509v2-abstract-full" style="display: none;"> A novel single-particle technique to measure emittance has been developed and used to characterise seventeen different muon beams for the Muon Ionisation Cooling Experiment (MICE). The muon beams, whose mean momenta vary from 171 to 281 MeV/c, have emittances of approximately 1.5--2.3 蟺mm-rad horizontally and 0.6--1.0 蟺mm-rad vertically, a horizontal dispersion of 90--190 mm and momentum spreads of about 25 MeV/c. There is reasonable agreement between the measured parameters of the beams and the results of simulations. The beams are found to meet the requirements of MICE. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1306.1509v2-abstract-full').style.display = 'none'; document.getElementById('1306.1509v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 October, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 June, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in EPJC, 20 pages, 15 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/1110.1813">arXiv:1110.1813</a> <span> [<a href="https://arxiv.org/pdf/1110.1813">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Accelerator Physics">physics.acc-ph</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"> MICE: the Muon Ionization Cooling Experiment. Step I: First Measurement of Emittance with Particle Physics Detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Bravar%2C+U">U. Bravar</a>, <a href="/search/physics?searchtype=author&query=Bogomilov%2C+M">M. Bogomilov</a>, <a href="/search/physics?searchtype=author&query=Karadzhov%2C+Y">Y. Karadzhov</a>, <a href="/search/physics?searchtype=author&query=Kolev%2C+D">D. Kolev</a>, <a href="/search/physics?searchtype=author&query=Russinov%2C+I">I. Russinov</a>, <a href="/search/physics?searchtype=author&query=Tsenov%2C+R">R. Tsenov</a>, <a href="/search/physics?searchtype=author&query=Wang%2C+L">L. Wang</a>, <a href="/search/physics?searchtype=author&query=Xu%2C+F+Y">F. Y. Xu</a>, <a href="/search/physics?searchtype=author&query=Zheng%2C+S+X">S. X. Zheng</a>, <a href="/search/physics?searchtype=author&query=Bertoni%2C+R">R. Bertoni</a>, <a href="/search/physics?searchtype=author&query=Bonesini%2C+M">M. Bonesini</a>, <a href="/search/physics?searchtype=author&query=Mazza%2C+R">R. Mazza</a>, <a href="/search/physics?searchtype=author&query=Palladino%2C+V">V. Palladino</a>, <a href="/search/physics?searchtype=author&query=Cecchet%2C+G">G. Cecchet</a>, <a href="/search/physics?searchtype=author&query=de+Bari%2C+A">A. de Bari</a>, <a href="/search/physics?searchtype=author&query=Capponi%2C+M">M. Capponi</a>, <a href="/search/physics?searchtype=author&query=Iaciofano%2C+A">A. Iaciofano</a>, <a href="/search/physics?searchtype=author&query=Orestano%2C+D">D. Orestano</a>, <a href="/search/physics?searchtype=author&query=Pastore%2C+F">F. Pastore</a>, <a href="/search/physics?searchtype=author&query=Tortora%2C+L">L. Tortora</a>, <a href="/search/physics?searchtype=author&query=Ishimoto%2C+S">S. Ishimoto</a>, <a href="/search/physics?searchtype=author&query=Suzuki%2C+S">S. Suzuki</a>, <a href="/search/physics?searchtype=author&query=Yoshimura%2C+K">K. Yoshimura</a>, <a href="/search/physics?searchtype=author&query=Mori%2C+Y">Y. Mori</a>, <a href="/search/physics?searchtype=author&query=Kuno%2C+Y">Y. Kuno</a> , et al. (123 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="1110.1813v2-abstract-short" style="display: inline;"> The Muon Ionization Cooling Experiment (MICE) is a strategic R&D project intended to demonstrate the only practical solution to providing high brilliance beams necessary for a neutrino factory or muon collider. MICE is under development at the Rutherford Appleton Laboratory (RAL) in the United Kingdom. It comprises a dedicated beamline to generate a range of input muon emittances and momenta, with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1110.1813v2-abstract-full').style.display = 'inline'; document.getElementById('1110.1813v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1110.1813v2-abstract-full" style="display: none;"> The Muon Ionization Cooling Experiment (MICE) is a strategic R&D project intended to demonstrate the only practical solution to providing high brilliance beams necessary for a neutrino factory or muon collider. MICE is under development at the Rutherford Appleton Laboratory (RAL) in the United Kingdom. It comprises a dedicated beamline to generate a range of input muon emittances and momenta, with time-of-flight and Cherenkov detectors to ensure a pure muon beam. The emittance of the incoming beam will be measured in the upstream magnetic spectrometer with a scintillating fiber tracker. A cooling cell will then follow, alternating energy loss in Liquid Hydrogen (LH2) absorbers to RF cavity acceleration. A second spectrometer, identical to the first, and a second muon identification system will measure the outgoing emittance. In the 2010 run at RAL the muon beamline and most detectors were fully commissioned and a first measurement of the emittance of the muon beam with particle physics (time-of-flight) detectors was performed. The analysis of these data was recently completed and is discussed in this paper. Future steps for MICE, where beam emittance and emittance reduction (cooling) are to be measured with greater accuracy, are also presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1110.1813v2-abstract-full').style.display = 'none'; document.getElementById('1110.1813v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 July, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 October, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Proceedings of the DPF-2011 Conference, Providence, RI, August 8-13, 2011</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" 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