22
views
0
recommends
+1 Recommend
0 collections
    0
    shares
      • Record: found
      • Abstract: found
      • Article: found
      Is Open Access

      Antiproton Flux, Antiproton-to-Proton Flux Ratio, and Properties of Elementary Particle Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the International Space Station.

      1 , 2 , 3 , 3 , 4 , 5 , 6 , 7 , 2 , 4 , 6 , 8 , 9 , 10 , 11 , 12 , 10 , 13 , 3 , 14 , 14 , 2 , 1 , 3 , 15 , 16 , 17 , 18 , 19 , 20 , 6 , 9 , 21 , 17 , 7 , 22 , 14 , 7 , 14 , 14 , 23 , 1 , 24 , 1 , 25 , 26 , 27 , 14 , 11 , 11 , 28 , 27 , 14 , 14 , 2 , 20 , 29 , 23 , 16 , 30 , 31 , 16 , 10 , 27 , 8 , 3 , 15 , 28 , 32 , 1 , 17 , 33 , 6 , 25 , 10 , 13 , 1 , 16 , 34 , 3 , 15 , 3 , 15 , 3 , 14 , 14 , 12 , 35 , 3 , 15 , 36 , 14 , 8 , 3 , 14 , 25 , 1 , 29 , 8 , 2 , 19 , 17 , 18 , 6 , 1 , 14 , 37 , 34 , 23 , 37 , 17 , 3 , 15 , 25 , 38 , 39 , 7 , 35 , 40 , 39 , 14 , 16 , 14 , 35 , 39 , 41 , 25 , 3 , 41 , 40 , 41 , 10 , 13 , 41 , 41 , 2 , 33 , 14 , 14 , 14 , 14 , 17 , 8 , 30 , 10 , 13 , 14 , 42 , 35 , 7 , 43 , 14 , 34 , 34 , 39 , 44 , 11 , 35 , 41 , 35 , 9 , 5 , 35 , 1 , 35 , 11 , 2 , 28 , 34 , 39 , 36 , 1 , 1 , 20 , 1 , 30 , 6 , 37 , 34 , 39 , 25 , 20 , 16 , 39 , 2 , 3 , 4 , 1 , 4 , 30 , 31 , 1 , 7 , 3 , 15 , 17 , 18 , 16 , 45 , 25 , 3 , 14 , 7 , 23 , 23 , 30 , 31 , 39 , 3 , 35 , 2 , 17 , 7 , 6 , 1 , 23 , 14 , 17 , 46 , 36 , 7 , 2 , 5 , 2 , 2 , 45 , 44 , 34 , 2 , 41 , 28 , 14 , 17 , 11 , 11 , 23 , 29 , 14 , 8 , 14 , 6 , 12 , 33 , 20 , 3 , 9 , 21 , 25 , 12 , 29 , 22 , 1 , 23 , 3 , 7 , 28 , 28 , 32 , 14 , 11 , 39 , 35 , 14 , 16 , 2 , 14 , 34 , 7 , 1 , 34 , 14 , 14 , 26 , 11 , 43 , 34 , 32 , 11 , 19 , 11 , 14 , 34 , 14 , 11 , 14 , 44 , 14 , 11 , 2 , 30 , 31 , 2 , 14
      Physical review letters
      American Physical Society (APS)

      Read this article at

      Bookmark
          There is no author summary for this article yet. Authors can add summaries to their articles on ScienceOpen to make them more accessible to a non-specialist audience.

          Abstract

          A precision measurement by AMS of the antiproton flux and the antiproton-to-proton flux ratio in primary cosmic rays in the absolute rigidity range from 1 to 450 GV is presented based on 3.49×10^{5} antiproton events and 2.42×10^{9} proton events. The fluxes and flux ratios of charged elementary particles in cosmic rays are also presented. In the absolute rigidity range ∼60 to ∼500  GV, the antiproton p[over ¯], proton p, and positron e^{+} fluxes are found to have nearly identical rigidity dependence and the electron e^{-} flux exhibits a different rigidity dependence. Below 60 GV, the (p[over ¯]/p), (p[over ¯]/e^{+}), and (p/e^{+}) flux ratios each reaches a maximum. From ∼60 to ∼500  GV, the (p[over ¯]/p), (p[over ¯]/e^{+}), and (p/e^{+}) flux ratios show no rigidity dependence. These are new observations of the properties of elementary particles in the cosmos.

          Related collections

          Most cited references76

          • Record: found
          • Abstract: found
          • Article: found
          Is Open Access

          Particle Dark Matter: Evidence, Candidates and Constraints

          In this review article, we discuss the current status of particle dark matter, including experimental evidence and theoretical motivations. We discuss a wide array of candidates for particle dark matter, but focus on neutralinos in models of supersymmetry and Kaluza-Klein dark matter in models of universal extra dimensions. We devote much of our attention to direct and indirect detection techniques, the constraints placed by these experiments and the reach of future experimental efforts.
            Bookmark
            • Record: found
            • Abstract: found
            • Article: found
            Is Open Access

            Supersymmetric Dark Matter

            There is almost universal agreement among astronomers that most of the mass in the Universe and most of the mass in the Galactic halo is dark. Many lines of reasoning suggest that the dark matter consists of some new, as yet undiscovered, weakly-interacting massive particle (WIMP). There is now a vast experimental effort being surmounted to detect WIMPS in the halo. The most promising techniques involve direct detection in low-background laboratory detectors and indirect detection through observation of energetic neutrinos from annihilation of WIMPs that have accumulated in the Sun and/or the Earth. Of the many WIMP candidates, perhaps the best motivated and certainly the most theoretically developed is the neutralino, the lightest superpartner in many supersymmetric theories. We review the minimal supersymmetric extension of the Standard Model and discuss prospects for detection of neutralino dark matter. We review in detail how to calculate the cosmological abundance of the neutralino and the event rates for both direct- and indirect-detection schemes, and we discuss astrophysical and laboratory constraints on supersymmetric models. We isolate and clarify the uncertainties from particle physics, nuclear physics, and astrophysics that enter at each step in the calculation. We briefly review other related dark-matter candidates and detection techniques.
              Bookmark
              • Record: found
              • Abstract: not found
              • Article: not found

              A multidimensional unfolding method based on Bayes' theorem

                Bookmark

                Author and article information

                Journal
                Phys. Rev. Lett.
                Physical review letters
                American Physical Society (APS)
                1079-7114
                0031-9007
                Aug 26 2016
                : 117
                : 9
                Affiliations
                [1 ] Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain.
                [2 ] I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany.
                [3 ] INFN Sezione di Perugia, I-06100 Perugia, Italy.
                [4 ] Laboratório de Instrumentação e Física Experimental de Partículas (LIP), P-1000 Lisboa, Portugal.
                [5 ] Jülich Supercomputing Centre and JARA-FAME, Research Centre Jülich, D-52425 Jülich, Germany.
                [6 ] Laboratoire de Physique Subatomique et de Cosmologie (LPSC), CNRS/IN2P3 and Université Grenoble-Alpes, F-38026 Grenoble, France.
                [7 ] DPNC, Université de Genève, CH-1211 Genève 4, Switzerland.
                [8 ] European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland.
                [9 ] INFN Sezione di Roma 1, I-00185 Roma, Italy.
                [10 ] INFN TIFPA, I-38123 Povo, Trento, Italy.
                [11 ] Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing, 100049, China.
                [12 ] Space Research Laboratory, Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland.
                [13 ] Università di Trento, I-38123 Povo, Trento, Italy.
                [14 ] Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA.
                [15 ] Università di Perugia, I-06100 Perugia, Italy.
                [16 ] Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA.
                [17 ] INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy.
                [18 ] Università di Milano-Bicocca, I-20126 Milano, Italy.
                [19 ] Institut für Experimentelle Kernphysik, Karlsruhe Institute of Technology (KIT), D-76128 Karlsruhe, Germany.
                [20 ] National Aeronautics and Space Administration Johnson Space Center (JSC), Jacobs Engineering, and Business Integra, Houston, Texas 77058, USA.
                [21 ] Università di Roma La Sapienza, I-00185 Roma, Italy.
                [22 ] Instituto de Fìsica de São Carlos, Universidade de São Paulo, CP 369, 13560-970, São Carlos, São Paulo, Brazil.
                [23 ] Laboratoire d'Annecy-le-Vieux de Physique des Particules (LAPP), CNRS/IN2P3 and Université Savoie Mont Blanc, F-74941 Annecy-le-Vieux, France.
                [24 ] CNR-IROE, I-50125 Firenze, Italy.
                [25 ] INFN Sezione di Pisa, I-56100 Pisa, Italy.
                [26 ] Department of Physics, Ewha Womans University, Seoul, 120-750, Korea.
                [27 ] National Central University (NCU), Chung-Li, Tao Yuan, 32054, Taiwan.
                [28 ] Shandong University (SDU), Jinan, Shandong, 250100, China.
                [29 ] Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, and Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain.
                [30 ] INFN Sezione di Bologna, I-40126 Bologna, Italy.
                [31 ] Università di Bologna, I-40126 Bologna, Italy.
                [32 ] Institute of Electrical Engineering (IEE), Chinese Academy of Sciences, Beijing, 100190, China.
                [33 ] Department of Physics, Middle East Technical University (METU), 06800 Ankara, Turkey.
                [34 ] Southeast University (SEU), Nanjing, 210096, China.
                [35 ] Institute of Physics, Academia Sinica, Nankang, Taipei 11529, Taiwan.
                [36 ] Physics Department, Yale University, New Haven, Connecticut 06520, USA.
                [37 ] Instituto de Física, Universidad Nacional Autónoma de México (UNAM), México, D. F., 01000 Mexico.
                [38 ] Università di Pisa, I-56100 Pisa, Italy.
                [39 ] Sun Yat-Sen University (SYSU), Guangzhou, 510275, China.
                [40 ] National Chung-Shan Institute of Science and Technology (NCSIST), Longtan, Tao Yuan, 32546, Taiwan.
                [41 ] CHEP, Kyungpook National University, 41566 Daegu, Korea.
                [42 ] Academia Sinica Grid Center (ASGC), Nankang, Taipei 11529, Taiwan.
                [43 ] National Cheng Kung University, Tainan, 70101, Taiwan.
                [44 ] Beihang University (BUAA), Beijing, 100191, China.
                [45 ] IPST, University of Maryland, College Park, Maryland 20742, USA.
                [46 ] East-West Center for Space Science, University of Maryland, College Park, Maryland 20742, USA.
                Article
                10.1103/PhysRevLett.117.091103
                27610839
                4229cf11-7872-4185-91a4-772c31086cc4
                History

                Comments

                Comment on this article