% IMPORTANT: The following is UTF-8 encoded.  This means that in the presence
% of non-ASCII characters, it will not work with BibTeX 0.99 or older.
% Instead, you should use an up-to-date BibTeX implementation like “bibtex8” or
% “biber”.

@ARTICLE{Aguilar:861500,
      author       = {Aguilar, M. and Ali Cavasonza, L. and Ambrosi, G. and
                      Arruda, L. and Attig, N. and Azzarello, P. and Bachlechner,
                      A. and Barao, F. and Barrau, A. and Barrin, L. and
                      Bartoloni, A. and Basara, L. and Başeğmez-du Pree, S. and
                      Battiston, R. and Becker, U. and Behlmann, M. and Beischer,
                      B. and Berdugo, J. and Bertucci, B. and Bindi, V. and de
                      Boer, W. and Bollweg, K. and Borgia, B. and Boschini, M. J.
                      and Bourquin, M. and Bueno, E. F. and Burger, J. and Burger,
                      W. J. and Cai, X. D. and Capell, M. and Caroff, S. and
                      Casaus, J. and Castellini, G. and Cervelli, F. and Chang, Y.
                      H. and Chen, G. M. and Chen, H. S. and Chen, Y. and Cheng,
                      L. and Chou, H. Y. and Choutko, V. and Chung, C. H. and
                      Clark, C. and Coignet, G. and Consolandi, C. and Contin, A.
                      and Corti, C. and Crispoltoni, M. and Cui, Z. and Dadzie, K.
                      and Dai, Y. M. and Datta, A. and Delgado, C. and Della
                      Torre, S. and Demirköz, M. B. and Derome, L. and Di Falco,
                      S. and Dimiccoli, F. and Díaz, C. and von Doetinchem, P.
                      and Dong, F. and Donnini, F. and Duranti, M. and Egorov, A.
                      and Eline, A. and Eronen, T. and Feng, J. and Fiandrini, E.
                      and Fisher, P. and Formato, V. and Galaktionov, Y. and
                      García-López, R. J. and Gargiulo, C. and Gast, H. and
                      Gebauer, I. and Gervasi, M. and Giovacchini, F. and
                      Gómez-Coral, D. M. and Gong, J. and Goy, C. and Grabski, V.
                      and Grandi, D. and Graziani, M. and Guo, K. H. and Haino, S.
                      and Han, K. C. and He, Z. H. and Heil, M. and Hsieh, T. H.
                      and Huang, H. and Huang, Z. C. and Incagli, M. and Jia, Yi
                      and Jinchi, H. and Kanishev, K. and Khiali, B. and Kirn, Th.
                      and Konak, C. and Kounina, O. and Kounine, A. and Koutsenko,
                      V. and Kulemzin, A. and La Vacca, G. and Laudi, E. and
                      Laurenti, G. and Lazzizzera, I. and Lebedev, A. and Lee, H.
                      T. and Lee, S. C. and Leluc, C. and Li, J. Q. and Li, Q. and
                      Li, T. X. and Li, Z. H. and Light, C. and Lin, C. H. and
                      Lippert, T. and Liu, F. Z. and Liu, Hu and Liu, Z. and Lu,
                      S. Q. and Lu, Y. S. and Luebelsmeyer, K. and Luo, F. and
                      Luo, J. Z. and Luo, Xi and Lyu, S. S. and Machate, F. and
                      Mañá, C. and Marín, J. and Martin, T. and Martínez, G.
                      and Masi, N. and Maurin, D. and Menchaca-Rocha, A. and Meng,
                      Q. and Mo, D. C. and Molero, M. and Mott, P. and Mussolin,
                      L. and Nelson, T. and Ni, J. Q. and Nikonov, N. and Nozzoli,
                      F. and Oliva, A. and Orcinha, M. and Palermo, M. and
                      Palmonari, F. and Paniccia, M. and Pashnin, A. and Pauluzzi,
                      M. and Pensotti, S. and Perrina, C. and Phan, H. D. and
                      Picot-Clemente, N. and Plyaskin, V. and Pohl, M. and
                      Poireau, V. and Popkow, A. and Quadrani, L. and Qi, X. M.
                      and Qin, X. and Qu, Z. Y. and Rancoita, P. G. and Rapin, D.
                      and Conde, A. Reina and Rosier-Lees, S. and Rozhkov, A. and
                      Rozza, D. and Sagdeev, R. and Solano, C. and Schael, S. and
                      Schmidt, Sebastian M. and Schulz von Dratzig, A. and
                      Schwering, G. and Seo, E. S. and Shan, B. S. and Shi, J. Y.
                      and Siedenburg, T. and Song, J. W. and Sun, Z. T. and
                      Tacconi, M. and Tang, X. W. and Tang, Z. C. and Tian, J. and
                      Ting, Samuel C. C. and Ting, S. M. and Tomassetti, N. and
                      Torsti, J. and Urban, T. and Vagelli, V. and Valente, E. and
                      Valtonen, E. and Vázquez Acosta, M. and Vecchi, M. and
                      Velasco, M. and Vialle, J. P. and Vizán, J. and Wang, L. Q.
                      and Wang, N. H. and Wang, Q. L. and Wang, X. and Wang, X. Q.
                      and Wang, Z. X. and Wei, J. and Weng, Z. L. and Wu, H. and
                      Xiong, R. Q. and Xu, W. and Yan, Q. and Yang, Y. and Yi, H.
                      and Yu, Y. J. and Yu, Z. Q. and Zannoni, M. and Zeissler, S.
                      and Zhang, C. and Zhang, F. and Zhang, J. H. and Zhang, Z.
                      and Zhao, F. and Zheng, Z. M. and Zhuang, H. L. and Zhukov,
                      V. and Zichichi, A. and Zimmermann, N. and Zuccon, P.},
      title        = {{T}owards {U}nderstanding the {O}rigin of {C}osmic-{R}ay
                      {P}ositrons},
      journal      = {Physical review letters},
      volume       = {122},
      number       = {4},
      issn         = {1079-7114},
      address      = {College Park, Md.},
      publisher    = {APS},
      reportid     = {FZJ-2019-01961},
      pages        = {041102},
      year         = {2019},
      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 $284^{+91}_{−64}  GeV$, (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 $E_s =810^{+310}_{−180}  GeV$ 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.},
      cin          = {JSC / VS-I / JARA-HPC},
      ddc          = {530},
      cid          = {I:(DE-Juel1)JSC-20090406 / I:(DE-Juel1)VS-I-20090406 /
                      $I:(DE-82)080012_20140620$},
      pnm          = {513 - Supercomputer Facility (POF3-513) / Cosmic-ray
                      physics with the AMS experiment on the International Space
                      Station $(jara0052_20150501)$},
      pid          = {G:(DE-HGF)POF3-513 / $G:(DE-Juel1)jara0052_20150501$},
      typ          = {PUB:(DE-HGF)16},
      pubmed       = {pmid:30768313},
      UT           = {WOS:000457061400002},
      doi          = {10.1103/PhysRevLett.122.041102},
      url          = {https://juser.fz-juelich.de/record/861500},
}