Properties of Daily Helium Fluxes

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2022-06-10

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Aguilar, M.
Cavasonza, L. Ali
Ambrosi, G.
Arruda, L.
Attig, N.
Barao, F.
Barrin, L.
Bartoloni, A.
Başeǧmez-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, Melahat Bilge
Derome, L.
Di Falco, S.
Di Felice, V.
Díaz, C.
Dimiccoli, F.
Von Doetinchem, P.
Dong, F.
Donnini, F.
Duranti, M.
Egorov, A.
Eline, A.
Feng, J.
Fiandrini, E.
Fisher, P.
Formato, V.
Freeman, C.
Gámez, C.
García-López, R.J.
Gargiulo, C.
Gast, H.
Gervasi, M.
Giovacchini, F.
Gómez-Coral, D.M.
Gong, J.
Goy, C.
Grabski, V.
Grandi, D.
Graziani, M.
Haino, S.
Han, K.C.
Hashmani, R.K.
He, Z.H.
Heber, B.
Hsieh, T.H.
Hu, J.Y.
Incagli, M.
Jang, W.Y.
Jia, Yi
Jinchi, H.
Karagöz, G.
Khiali, B.
Kim, G.N.
Kirn, Th.
Konyushikhin, M.
Kounina, O.
Kounine, A.
Koutsenko, V.
Krasnopevtsev, D.
Kuhlman, A.
Kulemzin, A.
La Vacca, G.
Laudi, E.
Laurenti, G.
Lazzizzera, I.
Lee, H.T.
Lee, S.C.
Li, H.L.
Li, J.Q.
Li, M.
Li, Q.
Li, Q.Y.
Li, S.
Li, S.L.
Li, J.H.
Li, Z.H.
Liang, J.
Liang, M.J.
Light, C.
Lin, C.H.
Lippert, T.
Liu, J.H.
Lu, S.Q.
Lu, Y.S.
Luebelsmeyer, K.
Luo, J.Z.
Luo, Xi
Machate, F.
Mañá, C.
Marín, J.
Marquardt, J.
Martin, T.
Martínez, G.
Masi, N.
Maurin, D.
Medvedeva, T.
Menchaca-Rocha, A.
Meng, Q.
Mikhailov, V.V.
Molero, M.
Mott, P.
Mussolin, L.
Negrete, J.
Nikonov, N.
Nozzoli, F.
Ocampo-Peleteiro, J.
Oliva, A.
Orcinha, M.
Palermo, M.
Palmonari, F.
Paniccia, M.
Pashnin, A.
Pauluzzi, M.
Pensotti, S.
Plyaskin, V.
Pohl, M.
Poluianov, S.
Qin, X.
Qu, Z.Y.
Quadrani, L.
Rancoita, P.G.
Rapin, D.
Conde, A. Reina
Robyn, E.
Rosier-Lees, S.
Rozhkov, A.
Rozza, D.
Sagdeev, R.
Schael, S.
Von Dratzig, A. Schultz
Schwering, G.
Seo, E.S.
Shan, B.S.
Siedenburg, T.
Song, J.W.
Song, X.J.
Sonnabend, R.
Strigari, L.
Su, T.
Sun, Q.
Sun, Z.T.
Tacconi, M.
Tang, X.W.
Tang, Z.C.
Tian, J.
Ting, Samuel C. C.
Ting, S.M.
Tomassetti, N.
Torsti, J.
Urban, T.
Usoskin, I.
Vagelli, V.
Vainio, R.
Valencia-Otero, M.
Valente, E.
Valtonen, E.
Vázquez Acosta, M.
Vecchi, M.
Velasco, M.
Vialle, J.P.
Wang, C.X.
Wang, L.
Wang, L.Q.
Wang, N.H.
Wang, Q.L.
Wang, S.
Wang, X.
Wang, Yu
Wang, Z.M.
Wei, J.
Weng, Z.L.
Wu, H.
Xiong, R.Q.
Xu, W.
Yan, Q.
Yang, Y.
Yashin, I.I.
Yi, H.
Yu, Y.M.
Yu, Z.Q.
Zannoni, M.
Zhang, C.
Zhang, F.
Zhang, F.Z.
Zhang, J.H.
Zhang, Z.
Zhao, F.
Zheng, C.
Zheng, Z.M.
Zhuang, H.L.
Zhukov, V.
Zichichi, A.
Zuccon, P.

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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.

URI

https://hdl.handle.net/11511/102479

Journal

Physical Review Letters

DOI

https://doi.org/10.1103/physrevlett.128.231102

Collections

Department of Physics, Article

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Properties of Neon, Magnesium, and Silicon Primary Cosmic Rays Results from the Alpha Magnetic Spectrometer Aguilar, M.; et. al. (American Physical Society (APS), 2020-05-29) We report the observation of new properties of primary cosmic rays, neon (Ne), magnesium (Mg), and silicon (Si), measured in the rigidity range 2.15 GV to 3.0 TV with 1.8 x 10(6) Ne, 2.2 x 10(6) Mg, and 1.6 x 10(6) Si nuclei collected by the Alpha Magnetic Spectrometer experiment on the International Space Station. The Ne and Mg spectra have identical rigidity dependence above 3.65 GV. The three spectra have identical rigidity dependence above 86.5 GV, deviate from a single power law above 200 GV, and harde...
Properties of Cosmic Helium Isotopes Measured by the Alpha Magnetic Spectrometer Aguilar, M.; et. al. (American Physical Society (APS), 2019-11-01) Precision measurements by the Alpha Magnetic Spectrometer (AMS) on the International Space Station of He-3 and He-4 fluxes are presented. The measurements are based on 100 million He-4 nuclei in the rigidity range from 2.1 to 21 GV and 18 million He-3 from 1.9 to 15 GV collected from May 2011 to November 2017. We observed that the He-3 and He-4 fluxes exhibit nearly identical variations with time. The relative magnitude of the variations decreases with increasing rigidity. The rigidity dependence of the He-...
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Towards Understanding the Origin of Cosmic-Ray Positrons Aguilar, M.; et. al. (American Physical Society (APS), 2019-01-29) Precision measurements of cosmic ray positrons are presented up to 1 TeV based on 1.9 million positrons collected by the Alpha Magnetic Spectrometer on the International Space Station. The positron flux exhibits complex energy dependence. Its distinctive properties are (a) a significant excess starting from 25.2 +/- 1.8 GeV compared to the lower-energy, power-law trend, (b) a sharp dropoff above 284(-64)(+91) GeV, (c) in the entire energy range the positron flux is well described by the sum of a term associ...

Citation Formats

M. Aguilar et al., “Properties of Daily Helium Fluxes,” Physical Review Letters, vol. 128, no. 23, pp. 0–0, 2022, Accessed: 00, 2023. [Online]. Available: https://hdl.handle.net/11511/102479.