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Periodicities in the Daily Proton Fluxes from 2011 to 2019 Measured by the Alpha Magnetic Spectrometer on the International Space Station from 1 to 100 GV.
Aguilar, M; Cavasonza, L Ali; Ambrosi, G; Arruda, L; Attig, N; Barao, F; Barrin, L; Bartoloni, A; Basegmez-du Pree, S; Battiston, R; Behlmann, M; Beranek, B; Berdugo, J; Bertucci, B; Bindi, V; Bollweg, K; Borgia, B; Boschini, M J; Bourquin, M; Bueno, E F; Burger, J; Burger, W J; Burmeister, S; Cai, X D; Capell, M; Casaus, J; Castellini, G; Cervelli, F; Chang, Y H; Chen, G M; Chen, G R; Chen, H S; Chen, Y; Cheng, L; Chou, H Y; Chouridou, S; Choutko, V; Chung, C H; Clark, C; Coignet, G; Consolandi, C; Contin, A; Corti, C; Cui, Z; Dadzie, K; Dass, A; Delgado, C; Della Torre, S; Demirköz, M B; Derome, L.
Afiliação
  • Aguilar M; Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 28040 Madrid, Spain.
  • Cavasonza LA; I. Physics Institute and JARA-FAME, RWTH Aachen University, 52056 Aachen, Germany.
  • Ambrosi G; INFN Sezione di Perugia, 06100 Perugia, Italy.
  • Arruda L; Laboratório de Instrumentação e Física Experimental de Partículas (LIP), 1649-003 Lisboa, Portugal.
  • Attig N; Jülich Supercomputing Centre and JARA-FAME, Research Centre Jülich, 52425 Jülich, Germany.
  • Barao F; Laboratório de Instrumentação e Física Experimental de Partículas (LIP), 1649-003 Lisboa, Portugal.
  • Barrin L; European Organization for Nuclear Research (CERN), 1211 Geneva 23, Switzerland.
  • Bartoloni A; INFN Sezione di Roma 1, 00185 Roma, Italy.
  • Basegmez-du Pree S; Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, Netherlands.
  • Battiston R; INFN TIFPA, 38123 Povo, Trento, Italy.
  • Behlmann M; Università di Trento, 38123 Povo, Trento, Italy.
  • Beranek B; Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
  • Berdugo J; I. Physics Institute and JARA-FAME, RWTH Aachen University, 52056 Aachen, Germany.
  • Bertucci B; Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 28040 Madrid, Spain.
  • Bindi V; INFN Sezione di Perugia, 06100 Perugia, Italy.
  • Bollweg K; Università di Perugia, 06100 Perugia, Italy.
  • Borgia B; Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA.
  • Boschini MJ; National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA.
  • Bourquin M; INFN Sezione di Roma 1, 00185 Roma, Italy.
  • Bueno EF; Università di Roma La Sapienza, 00185 Roma, Italy.
  • Burger J; INFN Sezione di Milano-Bicocca, 20126 Milano, Italy.
  • Burger WJ; DPNC, Université de Genève, 1211 Genève 4, Switzerland.
  • Burmeister S; Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, Netherlands.
  • Cai XD; Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
  • Capell M; INFN TIFPA, 38123 Povo, Trento, Italy.
  • Casaus J; Institut für Experimentelle und Angewandte Physik, Christian-Alberts-Universität zu Kiel, 24118 Kiel, Germany.
  • Castellini G; Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
  • Cervelli F; Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
  • Chang YH; Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 28040 Madrid, Spain.
  • Chen GM; CNR-IROE, 50125 Firenze, Italy.
  • Chen GR; INFN Sezione di Pisa, 56100 Pisa, Italy.
  • Chen HS; Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan.
  • Chen Y; Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China.
  • Cheng L; University of Chinese Academy of Sciences (UCAS), Beijing, 100049, China.
  • Chou HY; Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong, 250100, China.
  • Chouridou S; Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China.
  • Choutko V; University of Chinese Academy of Sciences (UCAS), Beijing, 100049, China.
  • Chung CH; DPNC, Université de Genève, 1211 Genève 4, Switzerland.
  • Clark C; Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong, 250100, China.
  • Coignet G; Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong, 250100, China.
  • Consolandi C; Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan.
  • Contin A; I. Physics Institute and JARA-FAME, RWTH Aachen University, 52056 Aachen, Germany.
  • Corti C; Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
  • Cui Z; I. Physics Institute and JARA-FAME, RWTH Aachen University, 52056 Aachen, Germany.
  • Dadzie K; Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
  • Dass A; National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA.
  • Delgado C; Université Grenoble Alpes, Université Savoie Mont Blanc, CNRS, LAPP-IN2P3, 74000 Annecy, France.
  • Della Torre S; Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA.
  • Demirköz MB; INFN Sezione di Bologna, 40126 Bologna, Italy.
  • Derome L; Università di Bologna, 40126 Bologna, Italy.
Phys Rev Lett ; 127(27): 271102, 2021 Dec 31.
Article em En | MEDLINE | ID: mdl-35061443
ABSTRACT
We present the precision measurement of the daily proton fluxes in cosmic rays from May 20, 2011 to October 29, 2019 (a total of 2824 days or 114 Bartels rotations) in the rigidity interval from 1 to 100 GV based on 5.5×10^{9} protons collected with the Alpha Magnetic Spectrometer aboard the International Space Station. The proton fluxes exhibit variations on multiple timescales. From 2014 to 2018, we observed recurrent flux variations with a period of 27 days. Shorter periods of 9 days and 13.5 days are observed in 2016. The strength of all three periodicities changes with time and rigidity. The rigidity dependence of the 27-day periodicity is different from the rigidity dependences of 9-day and 13.5-day periods. Unexpectedly, the strength of 9-day and 13.5-day periodicities increases with increasing rigidities up to ∼10 GV and ∼20 GV, respectively. Then the strength of the periodicities decreases with increasing rigidity up to 100 GV.

Texto completo: 1 Coleções: 01-internacional Base de dados: MEDLINE Idioma: En Revista: Phys Rev Lett Ano de publicação: 2021 Tipo de documento: Article País de afiliação: Espanha

Texto completo: 1 Coleções: 01-internacional Base de dados: MEDLINE Idioma: En Revista: Phys Rev Lett Ano de publicação: 2021 Tipo de documento: Article País de afiliação: Espanha