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Observation of Fine Time Structures in the Cosmic Proton and Helium Fluxes with the Alpha Magnetic Spectrometer on the International Space Station.
Aguilar, M; Ali Cavasonza, L; Alpat, B; Ambrosi, G; Arruda, L; Attig, N; Aupetit, S; Azzarello, P; Bachlechner, A; Barao, F; Barrau, A; Barrin, L; Bartoloni, A; Basara, L; Basegmez-du Pree, S; Battarbee, M; Battiston, R; Becker, U; Behlmann, M; Beischer, B; Berdugo, J; Bertucci, B; Bindel, K F; Bindi, V; de Boer, W; Bollweg, K; Bonnivard, V; Borgia, B; Boschini, M J; Bourquin, M; Bueno, E F; Burger, J; Cadoux, F; Cai, X D; Capell, M; Caroff, S; Casaus, J; Castellini, G; Cervelli, F; Chae, M J; Chang, Y H; Chen, A I; Chen, G M; Chen, H S; Chen, Y; Cheng, L; Chou, H Y; Choumilov, E; Choutko, V; Chung, C H.
Afiliación
  • Aguilar M; Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain.
  • Ali Cavasonza L; I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany.
  • Alpat B; INFN Sezione di Perugia, I-06100 Perugia, Italy.
  • Ambrosi G; INFN Sezione di Perugia, I-06100 Perugia, Italy.
  • Arruda L; Laboratório de Instrumentação e Física Experimental de Partículas (LIP), P-1000 Lisboa, Portugal.
  • Attig N; Jülich Supercomputing Centre and JARA-FAME, Research Centre Jülich, D-52425 Jülich, Germany.
  • Aupetit S; Laboratoire de Physique Subatomique et de Cosmologie (LPSC), CNRS/IN2P3 and Université Grenoble-Alpes, F-38026 Grenoble, France.
  • Azzarello P; DPNC, Université de Genève, CH-1211 Genève 4, Switzerland.
  • Bachlechner A; I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany.
  • Barao F; Laboratório de Instrumentação e Física Experimental de Partículas (LIP), P-1000 Lisboa, Portugal.
  • Barrau A; Laboratoire de Physique Subatomique et de Cosmologie (LPSC), CNRS/IN2P3 and Université Grenoble-Alpes, F-38026 Grenoble, France.
  • Barrin L; European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland.
  • Bartoloni A; INFN Sezione di Roma 1, I-00185 Roma, Italy.
  • Basara L; INFN TIFPA, I-38123 Povo, Trento, Italy.
  • Basegmez-du Pree S; Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China.
  • Battarbee M; Space Research Laboratory, Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland.
  • Battiston R; INFN TIFPA, I-38123 Povo, Trento, Italy.
  • Becker U; Università di Trento, I-38123 Povo, Trento, Italy.
  • Behlmann M; Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
  • Beischer B; Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
  • Berdugo J; I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany.
  • Bertucci B; Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain.
  • Bindel KF; INFN Sezione di Perugia, I-06100 Perugia, Italy.
  • Bindi V; Università di Perugia, I-06100 Perugia, Italy.
  • de Boer W; Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany.
  • Bollweg K; Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA.
  • Bonnivard V; Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany.
  • Borgia B; National Aeronautics and Space Administration Johnson Space Center (JSC), Jacobs Engineering, and Business Integra, Houston, Texas 77058, USA.
  • Boschini MJ; Laboratoire de Physique Subatomique et de Cosmologie (LPSC), CNRS/IN2P3 and Université Grenoble-Alpes, F-38026 Grenoble, France.
  • Bourquin M; INFN Sezione di Roma 1, I-00185 Roma, Italy.
  • Bueno EF; Università di Roma La Sapienza, I-00185 Roma, Italy.
  • Burger J; INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy.
  • Cadoux F; DPNC, Université de Genève, CH-1211 Genève 4, Switzerland.
  • Cai XD; Instituto de Física de São Carlos, Universidade de São Paulo, CP 369, 13560-970, São Carlos, São Paulo, SP, Brazil.
  • Capell M; Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
  • Caroff S; DPNC, Université de Genève, CH-1211 Genève 4, Switzerland.
  • Casaus J; Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
  • Castellini G; Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
  • Cervelli F; Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), CNRS/IN2P3 and Université Savoie Mont Blanc, F-74941 Annecy-le-Vieux, France.
  • Chae MJ; Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain.
  • Chang YH; CNR-IROE, I-50125 Firenze, Italy.
  • Chen AI; INFN Sezione di Pisa, I-56100 Pisa, Italy.
  • Chen GM; Department of Physics, Ewha Womans University, Seoul, 120-750, Korea.
  • Chen HS; National Central University (NCU), Chung-Li, Tao Yuan, 32054, Taiwan.
  • Chen Y; Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
  • Cheng L; Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China.
  • Chou HY; Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China.
  • Choumilov E; University of Chinese Academy of Sciences (UCAS), Beijing, 100049, China.
  • Choutko V; DPNC, Université de Genève, CH-1211 Genève 4, Switzerland.
  • Chung CH; Shandong University (SDU), Jinan, Shandong, 250100, China.
Phys Rev Lett ; 121(5): 051101, 2018 Aug 03.
Article en En | MEDLINE | ID: mdl-30118264
We present the precision measurement from May 2011 to May 2017 (79 Bartels rotations) of the proton fluxes at rigidities from 1 to 60 GV and the helium fluxes from 1.9 to 60 GV based on a total of 1×10^{9} events collected with the Alpha Magnetic Spectrometer aboard the International Space Station. This measurement is in solar cycle 24, which has the solar maximum in April 2014. We observed that, below 40 GV, the proton flux and the helium flux show nearly identical fine structures in both time and relative amplitude. The amplitudes of the flux structures decrease with increasing rigidity and vanish above 40 GV. The amplitudes of the structures are reduced during the time period, which started one year after solar maximum, when the proton and helium fluxes steadily increase. Above ∼3 GV the p/He flux ratio is time independent. We observed that below ∼3 GV the ratio has a long-term decrease coinciding with the period during which the fluxes start to rise.
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Texto completo: 1 Colección: 01-internacional Base de datos: MEDLINE Idioma: En Revista: Phys Rev Lett Año: 2018 Tipo del documento: Article País de afiliación: España Pais de publicación: Estados Unidos
Texto completo
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Texto completo: 1 Colección: 01-internacional Base de datos: MEDLINE Idioma: En Revista: Phys Rev Lett Año: 2018 Tipo del documento: Article País de afiliación: España Pais de publicación: Estados Unidos