Skip to main navigation Skip to search Skip to main content

Towards Understanding the Origin of Cosmic-Ray Positrons

  • M. Aguilar
  • , L. Ali Cavasonza
  • , G. Ambrosi
  • , L. Arruda
  • , N. Attig
  • , P. Azzarello
  • , A. Bachlechner
  • , F. Barao
  • , A. Barrau
  • , L. Barrin
  • , A. Bartoloni
  • , L. Basara
  • , S. Başeǧmez-Du Pree
  • , R. Battiston
  • , U. Becker
  • , M. Behlmann
  • , B. Beischer
  • , J. Berdugo
  • , B. Bertucci
  • , V. Bindi
  • W. De Boer, K. Bollweg, B. Borgia, M. J. Boschini, M. Bourquin, E. F. Bueno, J. Burger, W. J. Burger, X. D. Cai, M. Capell, S. Caroff, J. Casaus, G. Castellini, F. Cervelli, Y. H. Chang, G. M. Chen, H. S. Chen, Y. Chen, L. Cheng, H. Y. Chou, V. Choutko, C. H. Chung, C. Clark, G. Coignet, C. Consolandi, A. Contin, C. Corti, M. Crispoltoni, Z. Cui, K. Dadzie, Y. M. Dai, A. Datta, C. Delgado, S. Della Torre, M. B. Demirköz, L. Derome, S. Di Falco, F. Dimiccoli, C. Díaz, P. Von Doetinchem, F. Dong, F. Donnini, M. Duranti, A. Egorov, A. Eline, T. Eronen, J. Feng, E. Fiandrini, P. Fisher, V. Formato, Y. Galaktionov, R. J. García-López, C. Gargiulo, H. Gast, I. Gebauer, M. Gervasi, F. Giovacchini, D. M. Gómez-Coral, J. Gong, C. Goy, V. Grabski, D. Grandi, M. Graziani, K. H. Guo, S. Haino, K. C. Han, Z. H. He, M. Heil, T. H. Hsieh, H. Huang, Z. C. Huang, M. Incagli, Yi Jia, H. Jinchi, K. Kanishev, B. Khiali, Th Kirn, C. Konak, O. Kounina, A. Kounine, V. Koutsenko, A. Kulemzin, G. La Vacca, E. Laudi, G. Laurenti, I. Lazzizzera, A. Lebedev, H. T. Lee, S. C. Lee, C. Leluc, J. Q. Li, Q. Li, T. X. Li, Z. H. Li, C. Light, C. H. Lin, T. Lippert, F. Z. Liu, Hu Liu, Z. Liu, S. Q. Lu, Y. S. Lu, K. Luebelsmeyer, F. Luo, J. Z. Luo, Xi Luo, S. S. Lyu, F. MacHate, C. Mañá, J. Marín, T. Martin, G. Martínez, N. Masi, D. Maurin, A. Menchaca-Rocha, Q. Meng, D. C. Mo, M. Molero, P. Mott, L. Mussolin, T. Nelson, J. Q. Ni, N. Nikonov, F. Nozzoli, A. Oliva, M. Orcinha, M. Palermo, F. Palmonari, M. Paniccia, A. Pashnin, M. Pauluzzi, S. Pensotti, C. Perrina, H. D. Phan, N. Picot-Clemente, V. Plyaskin, M. Pohl, V. Poireau, A. Popkow, L. Quadrani, X. M. Qi, X. Qin, Z. Y. Qu, P. G. Rancoita, D. Rapin, A. Reina Conde, S. Rosier-Lees, A. Rozhkov, D. Rozza, R. Sagdeev, C. Solano, S. Schael, S. M. Schmidt, A. Schulz Von Dratzig, G. Schwering, E. S. Seo, B. S. Shan, J. Y. Shi, T. Siedenburg, J. W. Song, Z. T. Sun, M. Tacconi, X. W. Tang, Z. C. Tang, J. Tian, Samuel C.C. Ting, S. M. Ting, N. Tomassetti, J. Torsti, T. Urban, V. Vagelli, E. Valente, E. Valtonen, M. Vázquez Acosta, M. Vecchi, M. Velasco, J. P. Vialle, J. Vizán, L. Q. Wang, N. H. Wang, Q. L. Wang, X. Wang, X. Q. Wang, Z. X. Wang, J. Wei, Z. L. Weng, H. Wu, R. Q. Xiong, W. Xu, Q. Yan, Y. Yang, H. Yi, Y. J. Yu, Z. Q. Yu, M. Zannoni, S. Zeissler, C. Zhang, F. Zhang, J. H. Zhang, Z. Zhang, F. Zhao, Z. M. Zheng, H. L. Zhuang, V. Zhukov, A. Zichichi, N. Zimmermann, P. Zuccon
  • CIEMAT
  • RWTH Aachen University
  • National Institute for Nuclear Physics
  • Laboratório de Instrumentação e Física Experimental de Partículas
  • Jülich Research Centre
  • University of Geneva
  • Université Grenoble Alpes
  • CERN
  • University of Trento
  • University of Groningen
  • ASI
  • Massachusetts Institute of Technology
  • University of Perugia
  • University of Hawai'i at Mānoa
  • Karlsruhe Institute of Technology
  • NASA Johnson Space Center
  • University of Rome La Sapienza
  • Universidade de São Paulo
  • National Research Council of Italy
  • National Central University
  • CAS - Institute of High Energy Physics
  • University of Chinese Academy of Sciences
  • Shandong University
  • University of Bologna
  • CAS - Institute of Electrical Engineering
  • Middle East Technical University
  • Southeast University, Nanjing
  • ASI Space Science Data Center (SSDC)
  • University of Turku
  • University of La Laguna
  • University of Milan - Bicocca
  • Universidad Nacional Autónoma de México
  • Sun Yat-Sen University
  • Academia Sinica - Institute of Physics
  • Chung-shan Institute of Science and Technology Taiwan
  • Wuhan University
  • Academia Sinica Taiwan HQ
  • University of Maryland, College Park
  • Nankai University
  • National Cheng Kung University
  • Beihang University

Research output: Contribution to journalArticlepeer-review

Abstract

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 associated with the positrons produced in the collision of cosmic rays, which dominates at low energies, and a new source term of positrons, which dominates at high energies, and (d) a finite energy cutoff of the source term of Es=810-180+310 GeV is established with a significance of more than 4σ. These experimental data on cosmic ray positrons show that, at high energies, they predominantly originate either from dark matter annihilation or from other astrophysical sources.

Original languageEnglish
Article number041102
JournalPhysical Review Letters
Volume122
Issue number4
DOIs
StatePublished - 2019

Fingerprint

Dive into the research topics of 'Towards Understanding the Origin of Cosmic-Ray Positrons'. Together they form a unique fingerprint.

Cite this