Properties of Daily Helium Fluxes

(AMS Collaboration)

doi:10.1103/PhysRevLett.128.231102

Properties of Daily Helium Fluxes

(AMS Collaboration)

人工智能学院(人工智能研究院)

CIEMAT
RWTH Aachen University
National Institute for Nuclear Physics
Laboratório de Instrumentação e Física Experimental de Partículas
Jülich Research Centre
CERN
University of Groningen
National Institute for Subatomic Physics
University of Trento
Massachusetts Institute of Technology
University of Perugia
University of Hawai'i at Mānoa
NASA Johnson Space Center
University of Rome La Sapienza
University of Geneva
Kiel University
National Research Council of Italy
Academia Sinica - Institute of Physics
CAS - Institute of High Energy Physics
University of Chinese Academy of Sciences
Shandong Institute of Advanced Technology
Université Grenoble Alpes
University of Bologna
Shandong University
Middle East Technical University
ASI Space Science Data Center (SSDC)
Southeast University, Nanjing
Instituto de Astrofísica de Canarias
University of La Laguna
University of Milan - Bicocca
Universidad Nacional Autónoma de México
Chung-shan Institute of Science and Technology Taiwan
Sun Yat-Sen University
Kyungpook National University
Academia Sinica Taiwan HQ
CAS - Institute of Electrical Engineering
Moscow Engineering Physics Institute
University of Oulu
University of Maryland, College Park
Also at IRCCS Azienda Ospedaliero-Universitaria di Bologna
University of Turku
Italian Space Agency
National Central University
National Cheng Kung University
Beihang University

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49 引用（Scopus）

摘要

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 7.6×108 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.

源语言	英语
文章编号	231102
期刊	Physical Review Letters
卷	128
期	23
DOI	https://doi.org/10.1103/PhysRevLett.128.231102
出版状态	已出版 - 10 6月 2022

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@article{2969cf0e103548d399fcc01312b77350,

title = "Properties of Daily Helium Fluxes",

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 7.6×108 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.",

author = "\{(AMS Collaboration)\} and M. Aguilar and Cavasonza, \{L. Ali\} and G. Ambrosi and L. Arruda and N. Attig and F. Barao and L. Barrin and A. Bartoloni and \{Ba{\c s}eǧmez-Du Pree\}, S. and R. Battiston and M. Behlmann and J. Berdugo and B. Bertucci and V. Bindi and K. Bollweg and B. Borgia and Boschini, \{M. J.\} and M. Bourquin and Bueno, \{E. F.\} and J. Burger and Burger, \{W. J.\} and S. Burmeister and Cai, \{X. D.\} and M. Capell and J. Casaus and G. Castellini and F. Cervelli and Chang, \{Y. H.\} and Chen, \{G. M.\} and Chen, \{G. R.\} and Chen, \{H. S.\} and Y. Chen and L. Cheng and Chou, \{H. Y.\} and S. Chouridou and V. Choutko and Chung, \{C. H.\} and C. Clark and G. Coignet and C. Consolandi and A. Contin and C. Corti and Z. Cui and K. Dadzie and A. Dass and C. Delgado and \{Della Torre\}, S. and Demirk{\"o}z, \{M. B.\} and L. Derome and Shan, \{B. S.\}",

note = "Publisher Copyright: {\textcopyright} 2022 authors. Published by the American Physical Society.",

year = "2022",

month = jun,

day = "10",

doi = "10.1103/PhysRevLett.128.231102",

language = "英语",

volume = "128",

journal = "Physical Review Letters",

issn = "0031-9007",

publisher = "American Physical Society",

number = "23",

}

TY - JOUR

T1 - Properties of Daily Helium Fluxes

AU - (AMS Collaboration)

AU - Aguilar, M.

AU - Cavasonza, L. Ali

AU - Ambrosi, G.

AU - Arruda, L.

AU - Attig, N.

AU - Barao, F.

AU - Barrin, L.

AU - Bartoloni, A.

AU - Başeǧmez-Du Pree, S.

AU - Battiston, R.

AU - Behlmann, M.

AU - Berdugo, J.

AU - Bertucci, B.

AU - Bindi, V.

AU - Bollweg, K.

AU - Borgia, B.

AU - Boschini, M. J.

AU - Bourquin, M.

AU - Bueno, E. F.

AU - Burger, J.

AU - Burger, W. J.

AU - Burmeister, S.

AU - Cai, X. D.

AU - Capell, M.

AU - Casaus, J.

AU - Castellini, G.

AU - Cervelli, F.

AU - Chang, Y. H.

AU - Chen, G. M.

AU - Chen, G. R.

AU - Chen, H. S.

AU - Chen, Y.

AU - Cheng, L.

AU - Chou, H. Y.

AU - Chouridou, S.

AU - Choutko, V.

AU - Chung, C. H.

AU - Clark, C.

AU - Coignet, G.

AU - Consolandi, C.

AU - Contin, A.

AU - Corti, C.

AU - Cui, Z.

AU - Dadzie, K.

AU - Dass, A.

AU - Delgado, C.

AU - Della Torre, S.

AU - Demirköz, M. B.

AU - Derome, L.

AU - Shan, B. S.

PY - 2022/6/10

Y1 - 2022/6/10

N2 - 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 7.6×108 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.

AB - 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 7.6×108 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.

UR - https://www.scopus.com/pages/publications/85132341836

U2 - 10.1103/PhysRevLett.128.231102

DO - 10.1103/PhysRevLett.128.231102

M3 - 文章

C2 - 35749176

AN - SCOPUS:85132341836

SN - 0031-9007

VL - 128

JO - Physical Review Letters

JF - Physical Review Letters

IS - 23

M1 - 231102

ER -

Properties of Daily Helium Fluxes

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