Antiprotons and Elementary Particles over a Solar Cycle: Results from the Alpha Magnetic Spectrometer

作者：M. Aguilar, G. Ambrosi, H. R. Anderson, L. Arruda, N. Attig, C. Bagwell, F. Barão, M. Barbanera, L. Barrin, A. Bartoloni, R. Battiston, Ammar Bayyari, N. L. Belyaev, B. Bertucci, V. Bindi, K. Bollweg, J. Bolster, M. Borchiellini, B. Borgia, M. Boschini, M. Bourquin, C. Brugnoni, Johanna Bürger, W. J. Burger, X.D. Cai, M. Capell, J. Casaus, G. Castellini, F. Cervelli, Y. H. Chang, G. M. Chen, G. R. Chen, H. Chen, H. S. Chen, Y. Chen, Lin Cheng, H. Y. Chou, S. Chouridou, V. Choutko, C. H. Chung, C. Clark, G. Coignet, C. Consolandi, A. Contin, C. Corti, Z. Cui, S. Kokou Dadzie, Fulvio D’Angelo, Amala Dass, C. Delgado, S. Della Torre, B. Demirköz, L. Derome, S. Di Falco, V. Di Felice, C. Díaz, F. Dimiccoli, P. von Doetinchem, Fang Dong, M. Duranti, A. I. Egorov, A. Eline, F. Faldi, D. Fehr, J. H. Feng, E. Fiandrini, P.H. Fisher, V. Formato, R. J. Garcı́a López, C. Gargiulo, H. Gast, M. Gervasi, F. Giovacchini, D. M. Gómez-Coral, J. Gong, D. Grandi, M. Graziani, S. Haino, K. C. Han, R. K. Hashmani, Z. H. He, B. Heber, F. Hernández-Nicolás, Timothy H. Hsieh, Jiangyong Hu, B. W. Huang, M. Ionica, M. Incagli, Yi Jia, H. Jinchi, G. Karagöz, Th. Kirn, A. P. Klipfel, O. Kounina, A. Kounine, V. Koutsenko, D. Krasnopevtsev, A. Kuhlman, A. Kulemzin, G. La Vacca, E. Laudi, G. Laurenti, G. LaVecchia, I. Lazzizzera, H. T. Lee, S. C. Lee, H. L. Li, J. H. Li, Qiang Li, M. Li, M. Li, Q. Li, Q. Li, Q. Y. Li, S. Li, Shiliang Li, Z. H. Li, M. J. Liang, Pu Liao, Chao‐Hung Lin, Thomas Lippert, Haibo Liu, P. C. Liu, S. Q. Lu, Yao Lu, J. Luo, Q. Luo, Shan Luo, Xi Luo, C. Mañá, J. Marín, J. Marquardt, G. Martı́nez, N. Masi, D. Maurin, T. Medvedeva, A. Menchaca-Rocha, Q. Meng, V. V. Mikhailov, M. Molero, P. Mott, L. Mussolin, Y. Najafi Jozani, Riccardo Nicolaidis, N. Nikonov, F. Nozzoli, J. Ocampo-Peleteiro, A. Oliva, M. Orcinha, F. Palmonari, M. Paniccia, A. Pashnin, M. Pauluzzi, Dario Pelosi, S. Pensotti, P. Pietzcker, V. Plyaskin, Stepan Poluianov, D. Pridöhl, Z. H. Qu, L. Quadrani, P.G. Rancoita, D. Rapin, A. Reina Conde, E. Robyn, I. Rodríguez-García, Lisa Romaneehsen, F. Rossi, A. Rozhkov, D. Rozza, R. Z. Sagdeev, S. Schael, A. Schultz von Dratzig, G. Schwering, E. S. Seo, B. S. Shan, A. Shukla, T. Siedenburg, G. Silvestre, Jiwei Song, Xiaojian Song, R. Sonnabend, Lidia Strigari, T. Su, Qie Sun, Z. T. Sun, L. Tabarroni, M. Tacconi, Zichao Tang, Jie Tian, Y. Tian, Samuel C.C. Ting, S.M. Ting, Nicola Tomassetti, J. Torsti, Alessio Ubaldi, T. Urban, Ilya Usoskin, V. Vagelli, Rami Vainio, P. Väisänen, M. Valencia-Otero, E. Valente, E. Valtonen, M. Vázquez Acosta, M. Vecchi, M. Velasco, C. X. Wang, Jincheng Wang, L. Wang, L. Q. Wang, N. H. Wang, Q. L. Wang, S. Wang, X. Wang, Z. M. Wang, Chuncheng Wei, Z. Weng, H. Wu, Y. Wu, Zhibin Wu, J. N. Xiao, R. Q. Xiong, Xianze Xiong, W. Xu, Qi Yan, H. Yang, Y. Yang, Han Yi, Y. H. You, Young Moon Yu, Z. Q. Yu, C. Zhang, F. Z. Zhang, J. Zhang, J. H. Zhang, Z. Zhang, Pei Zhao, C. Zheng, Z. M. Zheng, H.L. Zhuang, V. Zhukov, A. Zichichi, M. Zuberi, P. Zuccon · 发表于：Physical Review Letters · 年份：2025 · DOI：10.1103/physrevlett.134.051002 · 被引用次数：18 · 研究领域：Dark Matter and Cosmic Phenomena、Solar and Space Plasma Dynamics、Atmospheric Ozone and Climate

We present results over an 11-year Solar cycle of cosmic antiprotons based on 1.1×10^{6} events in the rigidity range from 1.00 to 41.9 GV. The p[over ¯] fluxes exhibit distinct properties. The magnitude of the p[over ¯] flux temporal variation is significantly smaller than those of p, e^{-}, and e^{+}. A hysteresis between the p[over ¯] fluxes and the p fluxes is observed, whereas the p[over ¯] and e^{-} fluxes show a linear correlation. With a model-independent analysis, we found a universal relation between the shape of the rigidity spectrum and the magnitude of flux temporal variation over an 11-year Solar cycle for both positively and negatively charged particles. The simultaneous results on p[over ¯] and p, e^{-}, and e^{+} provide unique information for understanding particle transport in the Solar System as a function of mass, charge, and spectral shape.