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Properties of Daily Helium Fluxes.
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; 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; Di Falco, S.
Afiliación
  • 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.
  • 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.
  • 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.
  • Di Falco S; Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA.
Phys Rev Lett ; 128(23): 231102, 2022 Jun 10.
Article en En | MEDLINE | ID: mdl-35749176
ABSTRACT
We present the precision measurement of 2824 daily helium fluxes in cosmic rays from May 20, 2011 to October 29, 2019 in the rigidity interval from 1.71 to 100 GV based on 7.6×10^{8} helium nuclei collected with the Alpha Magnetic Spectrometer (AMS) aboard the International Space Station. The helium flux and the helium to proton flux ratio exhibit variations on multiple timescales. In nearly all the time intervals from 2014 to 2018, we observed recurrent helium 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. In the entire time period, we found that below ∼7 GV the helium flux exhibits larger time variations than the proton flux, and above ∼7 GV the helium to proton flux ratio is time independent. Remarkably, below 2.4 GV a hysteresis between the helium to proton flux ratio and the helium flux was observed at greater than the 7σ level. This shows that at low rigidity the modulation of the helium to proton flux ratio is different before and after the solar maximum in 2014.
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Texto completo: 1 Colección: 01-internacional Banco de datos: MEDLINE Idioma: En Revista: Phys Rev Lett Año: 2022 Tipo del documento: Article País de afiliación: España
Texto completo
Imprimir
XML
PubMed Links
Buscar en Google

Texto completo: 1 Colección: 01-internacional Banco de datos: MEDLINE Idioma: En Revista: Phys Rev Lett Año: 2022 Tipo del documento: Article País de afiliación: España