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Temporal Structures in Positron Spectra and Charge-Sign Effects in Galactic Cosmic Rays.
Aguilar, M; Ambrosi, G; Anderson, H; Arruda, L; Attig, N; Bagwell, C; Barao, F; Barbanera, M; Barrin, L; Bartoloni, A; Battiston, R; Belyaev, N; Berdugo, J; Bertucci, B; Bindi, V; Bollweg, K; Bolster, J; Borchiellini, M; Borgia, B; Boschini, M J; Bourquin, M; Burger, J; Burger, W J; Cai, X D; Capell, M; Casaus, J; Castellini, G; Cervelli, F; Chang, Y H; Chen, G M; Chen, G R; Chen, H; 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; D'Angelo, F; Dass, A; Delgado, C; Della Torre, S.
Afiliação
  • Aguilar M; Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), 28040 Madrid, Spain.
  • Ambrosi G; INFN Sezione di Perugia, 06100 Perugia, Italy.
  • Anderson H; Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
  • 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.
  • Bagwell C; Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
  • Barao F; Laboratório de Instrumentação e Física Experimental de Partículas (LIP), 1649-003 Lisboa, Portugal.
  • Barbanera M; INFN Sezione di Perugia, 06100 Perugia, Italy.
  • Barrin L; European Organization for Nuclear Research (CERN), 1211 Geneva 23, Switzerland.
  • Bartoloni A; INFN Sezione di Roma 1, 00185 Roma, Italy.
  • Battiston R; INFN TIFPA, 38123 Trento, Italy.
  • Belyaev N; Università di Trento, 38123 Trento, Italy.
  • Berdugo J; Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
  • 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.
  • Bolster J; Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA.
  • Borchiellini M; National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA.
  • Borgia B; Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
  • Boschini MJ; Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, Netherlands.
  • Bourquin M; INFN Sezione di Roma 1, 00185 Roma, Italy.
  • Burger J; Università di Roma La Sapienza, 00185 Roma, Italy.
  • Burger WJ; INFN Sezione di Milano-Bicocca, 20126 Milano, Italy.
  • Cai XD; DPNC, Université de Genève, 1211 Genève 4, Switzerland.
  • Capell M; Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
  • Casaus J; INFN TIFPA, 38123 Trento, Italy.
  • 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 H; Institute of Physics, Academia Sinica, Nankang, Taipei 11529, Taiwan.
  • Chen HS; Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China.
  • Chen Y; University of Chinese Academy of Sciences (UCAS), Beijing 100049, China.
  • Cheng L; Shandong Institute of Advanced Technology (SDIAT), Jinan, Shandong 250100, China.
  • Chou HY; Zhejiang University (ZJU), Hangzhou 310058, 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.
  • D'Angelo F; National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA.
  • Dass A; Université Grenoble Alpes, Université Savoie Mont Blanc, CNRS, LAPP-IN2P3, 74000 Annecy, France.
  • Delgado C; Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA.
  • Della Torre S; INFN Sezione di Bologna, 40126 Bologna, Italy.
Phys Rev Lett ; 131(15): 151002, 2023 Oct 13.
Article em En | MEDLINE | ID: mdl-37897756
ABSTRACT
We present the precision measurements of 11 years of daily cosmic positron fluxes in the rigidity range from 1.00 to 41.9 GV based on 3.4×10^{6} positrons collected with the Alpha Magnetic Spectrometer (AMS) aboard the International Space Station. The positron fluxes show distinctly different time variations from the electron fluxes at short and long timescales. A hysteresis between the electron fluxes and the positron fluxes is observed with a significance greater than 5σ at rigidities below 8.5 GV. On the contrary, the positron fluxes and the proton fluxes show similar time variation. Remarkably, we found that positron fluxes are modulated more than proton fluxes with a significance greater than 5σ for rigidities below 7 GV. These continuous daily positron fluxes, together with AMS daily electron, proton, and helium fluxes over an 11-year solar cycle, provide unique input to the understanding of both the charge-sign and mass dependencies of cosmic rays in the heliosphere.
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Texto completo: 1 Base de dados: MEDLINE Idioma: En Ano de publicação: 2023 Tipo de documento: Article
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Texto completo: 1 Base de dados: MEDLINE Idioma: En Ano de publicação: 2023 Tipo de documento: Article