1
|
Fornieri O, Gaggero D, Guberman D, Brahimi L, Luque PDLT, Marcowith A. Diffusive origin for the cosmic-ray spectral hardening reveals signatures of a nearby source in the leptons and protons data. Int J Clin Exp Med 2021. [DOI: 10.1103/physrevd.104.103013] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
2
|
Abstract
We review numerical methods for simulations of cosmic ray (CR) propagation on galactic and larger scales. We present the development of algorithms designed for phenomenological and self-consistent models of CR propagation in kinetic description based on numerical solutions of the Fokker–Planck equation. The phenomenological models assume a stationary structure of the galactic interstellar medium and incorporate diffusion of particles in physical and momentum space together with advection, spallation, production of secondaries and various radiation mechanisms. The self-consistent propagation models of CRs include the dynamical coupling of the CR population to the thermal plasma. The CR transport equation is discretized and solved numerically together with the set of MHD equations in various approaches treating the CR population as a separate relativistic fluid within the two-fluid approach or as a spectrally resolved population of particles evolving in physical and momentum space. The relevant processes incorporated in self-consistent models include advection, diffusion and streaming propagation as well as adiabatic compression and several radiative loss mechanisms. We discuss, applications of the numerical models for the interpretation of CR data collected by various instruments. We present example models of astrophysical processes influencing galactic evolution such as galactic winds, the amplification of large-scale magnetic fields and instabilities of the interstellar medium.
Collapse
|
3
|
Phan VHM, Schulze F, Mertsch P, Recchia S, Gabici S. Stochastic Fluctuations of Low-Energy Cosmic Rays and the Interpretation of Voyager Data. Phys Rev Lett 2021; 127:141101. [PMID: 34652203 DOI: 10.1103/physrevlett.127.141101] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/04/2021] [Revised: 06/25/2021] [Accepted: 08/17/2021] [Indexed: 06/13/2023]
Abstract
Data from the Voyager probes have provided us with the first measurement of cosmic ray intensities at MeV energies, an energy range that had previously not been explored. Simple extrapolations of models that fit data at GeV energies, e.g., from AMS-02, however, fail to reproduce the Voyager data in that the predicted intensities are too high. Oftentimes, this discrepancy is addressed by adding a break to the source spectrum or the diffusion coefficient in an ad hoc fashion, with a convincing physical explanation yet to be provided. Here, we argue that the discrete nature of cosmic ray sources, which is usually ignored, is instead a more likely explanation. We model the distribution of intensities expected from a statistical model of discrete sources and show that its expectation value is not representative but has a spectral shape different from that for a typical configuration of sources. The Voyager proton and electron data are however compatible with the median of the intensity distribution.
Collapse
Affiliation(s)
- Vo Hong Minh Phan
- Institute for Theoretical Particle Physics and Cosmology (TTK), RWTH Aachen University, Aachen 52056, Germany
- Université de Paris, CNRS, Astroparticule et Cosmologie, Paris F-75006, France
| | - Florian Schulze
- Institute for Theoretical Particle Physics and Cosmology (TTK), RWTH Aachen University, Aachen 52056, Germany
| | - Philipp Mertsch
- Institute for Theoretical Particle Physics and Cosmology (TTK), RWTH Aachen University, Aachen 52056, Germany
| | - Sarah Recchia
- Dipartimento di Fisica, Universitá di Torino, via P. Giuria 1, Torino 10125, Italy
| | - Stefano Gabici
- Université de Paris, CNRS, Astroparticule et Cosmologie, Paris F-75006, France
| |
Collapse
|
4
|
Boschini MJ, Della Torre S, Gervasi M, Grandi D, Jóhannesson G, La Vacca G, Masi N, Moskalenko IV, Pensotti S, Porter TA, Quadrani L, Rancoita PG, Rozza D, Tacconi M. The Discovery of a Low-energy Excess in Cosmic-Ray Iron: Evidence of the Past Supernova Activity in the Local Bubble. Astrophys J 2021; 913:5. [PMID: 34646050 PMCID: PMC8506974 DOI: 10.3847/1538-4357/abf11c] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/12/2023]
Abstract
Since its launch, the Alpha Magnetic Spectrometer-02 (AMS-02) has delivered outstanding quality measurements of the spectra of cosmic-ray (CR) species ( p ¯ , e ±, and nuclei, 1H-8O, 10Ne, 12Mg, 14Si) which resulted in a number of breakthroughs. One of the latest long-awaited surprises is the spectrum of 26Fe just published by AMS-02. Because of the large fragmentation cross section and large ionization energy losses, most of CR iron at low energies is local and may harbor some features associated with relatively recent supernova (SN) activity in the solar neighborhood. Our analysis of the new AMS-02 results, together with Voyager 1 and ACE-CRIS data, reveals an unexpected bump in the iron spectrum and in the Fe/He, Fe/O, and Fe/Si ratios at 1-2 GV, while a similar feature in the spectra of He, O, and Si and in their ratios is absent, hinting at a local source of low-energy CRs. The found excess extends the recent discoveries of radioactive 60Fe deposits in terrestrial and lunar samples and in CRs. We provide an updated local interstellar spectrum (LIS) of iron in the energy range from 1 MeV nucleon-1 to ~10 TeV nucleon-1. Our calculations employ the GALPROP-HELMOD framework, which has proved to be a reliable tool in deriving the LIS of CR p ¯ , e -, and nuclei Z ⩽ 28.
Collapse
Affiliation(s)
- M J Boschini
- INFN, Milano-Bicocca, Milano, Italy
- CINECA, Segrate, Milano, Italy
| | | | - M Gervasi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - D Grandi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - G Jóhannesson
- Science Institute, University of Iceland, Dunhaga 3, IS-107 Reykjavik, Iceland
- NORDITA, Roslagstullsbacken 23, SE-106 91 Stockholm, Sweden
| | - G La Vacca
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - N Masi
- INFN, Bologna, Italy
- Physics Department, University of Bologna, Bologna, Italy
| | - I V Moskalenko
- Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - S Pensotti
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - T A Porter
- Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - L Quadrani
- INFN, Bologna, Italy
- Physics Department, University of Bologna, Bologna, Italy
| | | | - D Rozza
- INFN, Milano-Bicocca, Milano, Italy
| | - M Tacconi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| |
Collapse
|
5
|
Motz H, Okada H, Asaoka Y, Kohri K. Cosmic-ray signatures of dark matter from a flavor dependent gauge symmetry model with neutrino mass mechanism. Int J Clin Exp Med 2020. [DOI: 10.1103/physrevd.102.083019] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
6
|
Boschini MJ, Torre SD, Gervasi M, Grandi D, Jóhannesson G, La Vacca G, Masi N, Moskalenko IV, Pensotti S, Porter TA, Quadrani L, Rancoita PG, Rozza D, Tacconi M. Inference of the Local Interstellar Spectra of Cosmic-Ray Nuclei Z ⩽ 28 with the GalProp-HelMod Framework. Astrophys J Suppl Ser 2020; 250:27. [PMID: 34711999 PMCID: PMC8549769 DOI: 10.3847/1538-4365/aba901] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/08/2023]
Abstract
Composition and spectra of Galactic cosmic rays (CRs) are vital for studies of high-energy processes in a variety of environments and on different scales, for interpretation of γ-ray and microwave observations, for disentangling possible signatures of new phenomena, and for understanding of our local Galactic neighborhood. Since its launch, AMS-02 has delivered outstanding-quality measurements of the spectra of p ¯ , e ±, and nuclei: 1H-8O, 10Ne, 12Mg, 14Si. These measurements resulted in a number of breakthroughs; however, spectra of heavier nuclei and especially low-abundance nuclei are not expected until later in the mission. Meanwhile, a comparison of published AMS-02 results with earlier data from HEAO-3-C2 indicates that HEAO-3-C2 data may be affected by undocumented systematic errors. Utilizing such data to compensate for the lack of AMS-02 measurements could result in significant errors. In this paper we show that a fraction of HEAO-3-C2 data match available AMS-02 measurements quite well and can be used together with Voyager 1 and ACE-CRIS data to make predictions for the local interstellar spectra (LIS) of nuclei that are not yet released by AMS-02. We are also updating our already-published LIS to provide a complete set from 1H-28Ni in the energy range from 1 MeV nucleon-1 to ~100-500 TeV nucleon-1, thus covering 8-9 orders of magnitude in energy. Our calculations employ the GalProp-HelMod framework, which has proved to be a reliable tool in deriving the LIS of CR p ¯ , e -, and nuclei 1H-8O.
Collapse
Affiliation(s)
- M J Boschini
- INFN, Milano-Bicocca, Milano, Italy
- CINECA, Segrate, Milano, Italy
| | | | - M Gervasi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - D Grandi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - G Jóhannesson
- Science Institute, University of Iceland, Dunhaga 3, IS-107 Reykjavik, Iceland
- NORDITA, Roslagstullsbacken 23, 106 91 Stockholm, Sweden
| | - G La Vacca
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - N Masi
- INFN, Bologna, Italy
- Physics Department, University of Bologna, Bologna, Italy
| | - I V Moskalenko
- Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - S Pensotti
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - T A Porter
- Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - L Quadrani
- INFN, Bologna, Italy
- Physics Department, University of Bologna, Bologna, Italy
| | | | - D Rozza
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - M Tacconi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| |
Collapse
|
7
|
Maurin D, Dembinski HP, Gonzalez J, Mariş IC, Melot F. Cosmic-Ray Database Update: Ultra-High Energy, Ultra-Heavy, and Antinuclei Cosmic-Ray Data (CRDB v4.0). Universe 2020; 6:102. [DOI: 10.3390/universe6080102] [Citation(s) in RCA: 16] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
We present an update on CRDB, the cosmic-ray database for charged species. CRDB is based on MySQL, queried and sorted by jquery and table-sorter libraries, and displayed via PHP web pages through the AJAX protocol. We review the modifications made on the structure and outputs of the database since the first release (Maurin et al., 2014). For this update, the most important feature is the inclusion of ultra-heavy nuclei (Z>30), ultra-high energy nuclei (from 1015 to 1020 eV), and limits on antinuclei fluxes (Z≤−1 for A>1); more than 100 experiments, 350 publications, and 40,000 data points are now available in CRDB. We also revisited and simplified how users can retrieve data and submit new ones. For questions and requests, please contact crdb@lpsc.in2p3.fr.
Collapse
|
8
|
Wang X, Li Z, Tang Z, Zhang C, Zhao F, Sun Z, Zhang F, Hu J, Chen G, Chen H. Improvement in the 3D shower shapes description in the Monte Carlo simulation for a lead-scintillating fiber electromagnetic calorimeter. Radiat Detect Technol Methods 2019; 3:34. [DOI: 10.1007/s41605-019-0113-3] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 10/27/2022]
|
9
|
Abstract
The Andromeda galaxy is the closest spiral galaxy to us and has been the subject of numerous studies. It harbors a massive dark matter halo, which may span up to ~600 kpc across and comprises ~90% of the galaxy's total mass. This halo size translates into a large diameter of 42° on the sky, for an M31-Milky Way (MW) distance of 785 kpc, but its presumably low surface brightness makes it challenging to detect with γ-ray telescopes. Using 7.6 yr of Fermi Large Area Telescope (Fermi-LAT) observations, we make a detailed study of the γ-ray emission between 1-100 GeV toward M31's outer halo, with a total field radius of 60° centered at M31, and perform an in-depth analysis of the systematic uncertainties related to the observations. We use the cosmic-ray propagation code GALPROP to construct specialized interstellar emission models to characterize the foreground γ-ray emission from the MW, including a self-consistent determination of the isotropic component. We find evidence for an extended excess that appears to be distinct from the conventional MW foreground, having a total radial extension upward of ~120-200 kpc from the center of M31. We discuss plausible interpretations of the excess emission, but emphasize that uncertainties in the MW foreground-and in particular, modeling of the H i-related components-have not been fully explored and may impact the results.
Collapse
Affiliation(s)
- Christopher M Karwin
- Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA
| | - Simona Murgia
- Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA
| | - Sheldon Campbell
- Department of Physics and Astronomy, University of California, Irvine, CA 92697, USA
| | - Igor V Moskalenko
- Hansen Experimental Physics Laboratory and Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| |
Collapse
|
10
|
Xi S, Liu R, Huang Z, Fang K, Wang X. GeV Observations of the Extended Pulsar Wind Nebulae Constrain the Pulsar Interpretations of the Cosmic-Ray Positron Excess. ACTA ACUST UNITED AC 2019; 878:104. [DOI: 10.3847/1538-4357/ab20c9] [Citation(s) in RCA: 23] [Impact Index Per Article: 4.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
|
11
|
Abstract
The High Energy cosmic-Radiation Detection (HERD) facility will be one of the space astronomy payloads on board the future Chinese space station. The ambitious aim of HERD is the direct detection of cosmic rays towards the “knee” region (~ 1 PeV), with a detector able to measure electrons, photons and nuclei with an excellent energy resolution (1% for electrons and photons at 200 GeV and 20% for nuclei at 100 GeV - PeV), an acceptance 10 times the one of present generation missions (~ 1 m2 sr), and long life-time (> 10 years). The primary objectives of HERD are the indirect search for dark matter particles and the precise measurement of energy distribution and composition of cosmic rays from 30 GeV up to a few PeV, determining the origin of the “knee” structure of the spectrum. Furthermore, HERD will monitor the high energy gamma-ray sky from 500 MeV, observing gamma-ray bursts, active galactic nuclei, galactic microquasars, etc. HERD will be composed of a homogeneous calorimeter, surrounded by a particle tracker and a plastic scintillator detector. Two possible trackers are under study: a 5-side tracker made of silicon strip detectors and a 4-side scintillating fiber tracker with a silicon strip top tracker. The total volume of HERD will be (2.3 × 2.3 × 2.6) m3 with a weight of about 4 t. The HERD design, perspectives, expected performances in terms of energy sensitivity and acceptance will be presented in this contribution.
Collapse
|
12
|
Aguilar M, Ali Cavasonza L, Alpat B, Ambrosi G, Arruda L, Attig N, Azzarello P, Bachlechner A, Barao F, Barrau A, Barrin L, Bartoloni A, Basara L, Başeğmez-du Pree S, Battiston R, Becker U, Behlmann M, Beischer B, Berdugo J, Bertucci B, Bindi V, de Boer W, Bollweg K, Borgia B, Boschini MJ, Bourquin M, Bueno EF, Burger J, Burger WJ, Cai XD, Capell M, Caroff S, Casaus J, Castellini G, Cervelli F, Chang YH, Chen GM, Chen HS, Chen Y, Cheng L, Chou HY, Choutko V, Chung CH, Clark C, Coignet G, Consolandi C, Contin A, Corti C, Crispoltoni M, Cui Z, Dadzie K, Dai YM, Datta A, Delgado C, Della Torre S, Demirköz MB, Derome L, Di Falco S, Di Felice V, Dimiccoli F, Díaz C, von Doetinchem P, Dong F, Donnini F, Duranti M, Egorov A, Eline A, Eronen T, Feng J, Fiandrini E, Fisher P, Formato V, Galaktionov Y, García-López RJ, Gargiulo C, Gast H, Gebauer I, Gervasi M, Giovacchini F, Gómez-Coral DM, Gong J, Goy C, Grabski V, Grandi D, Graziani M, Guo KH, Haino S, Han KC, He ZH, Heil M, Hsieh TH, Huang H, Huang ZC, Incagli M, Jia Y, Jinchi H, Kanishev K, Khiali B, Kirn T, Konak C, Kounina O, Kounine A, Koutsenko V, Kulemzin A, La Vacca G, Laudi E, Laurenti G, Lazzizzera I, Lebedev A, Lee HT, Lee SC, Leluc C, Li JQ, Li Q, Li TX, Li ZH, Light C, Lin CH, Lippert T, Liu FZ, Liu H, Liu Z, Lu SQ, Lu YS, Luebelsmeyer K, Luo F, Luo JZ, Luo X, Lyu SS, Machate F, Mañá C, Marín J, Martin T, Martínez G, Masi N, Maurin D, Menchaca-Rocha A, Meng Q, Mo DC, Molero M, Mott P, Mussolin L, Nelson T, Ni JQ, Nikonov N, Nozzoli F, Oliva A, Orcinha M, Palermo M, Palmonari F, Paniccia M, Pashnin A, Pauluzzi M, Pensotti S, Perrina C, Phan HD, Picot-Clemente N, Plyaskin V, Pohl M, Poireau V, Popkow A, Quadrani L, Qi XM, Qin X, Qu ZY, Rancoita PG, Rapin D, Conde AR, Rosier-Lees S, Rozhkov A, Rozza D, Sagdeev R, Solano C, Schael S, Schmidt SM, von Dratzig AS, Schwering G, Seo ES, Shan BS, Shi JY, Siedenburg T, Song JW, Sun ZT, Tacconi M, Tang XW, Tang ZC, Tian J, Ting SCC, Ting SM, Tomassetti N, Torsti J, Urban T, Vagelli V, Valente E, Valtonen E, Acosta MV, Vecchi M, Velasco M, Vialle JP, Vizán J, Wang LQ, Wang NH, Wang QL, Wang X, Wang XQ, Wang ZX, Wei J, Weng ZL, Wu H, Xiong RQ, Xu W, Yan Q, Yang Y, Yi H, Yu YJ, Yu ZQ, Zannoni M, Zeissler S, Zhang C, Zhang F, Zhang JH, Zhang Z, Zhao F, Zheng ZM, Zhuang HL, Zhukov V, Zichichi A, Zimmermann N, Zuccon P. Towards Understanding the Origin of Cosmic-Ray Electrons. Phys Rev Lett 2019; 122:101101. [PMID: 30932626 DOI: 10.1103/physrevlett.122.101101] [Citation(s) in RCA: 19] [Impact Index Per Article: 3.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/07/2019] [Indexed: 06/09/2023]
Abstract
Precision results on cosmic-ray electrons are presented in the energy range from 0.5 GeV to 1.4 TeV based on 28.1×10^{6} electrons collected by the Alpha Magnetic Spectrometer on the International Space Station. In the entire energy range the electron and positron spectra have distinctly different magnitudes and energy dependences. The electron flux exhibits a significant excess starting from 42.1_{-5.2}^{+5.4} GeV compared to the lower energy trends, but the nature of this excess is different from the positron flux excess above 25.2±1.8 GeV. Contrary to the positron flux, which has an exponential energy cutoff of 810_{-180}^{+310} GeV, at the 5σ level the electron flux does not have an energy cutoff below 1.9 TeV. In the entire energy range the electron flux is well described by the sum of two power law components. The different behavior of the cosmic-ray electrons and positrons measured by the Alpha Magnetic Spectrometer is clear evidence that most high energy electrons originate from different sources than high energy positrons.
Collapse
Affiliation(s)
- M Aguilar
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - L Ali Cavasonza
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - B Alpat
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - G Ambrosi
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - L Arruda
- Laboratório de Instrumentação e Física Experimental de Partículas (LIP), P-1000 Lisboa, Portugal
| | - N Attig
- Jülich Supercomputing Centre and JARA-FAME, Research Centre Jülich, D-52425 Jülich, Germany
| | - P Azzarello
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - A Bachlechner
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - F Barao
- Laboratório de Instrumentação e Física Experimental de Partículas (LIP), P-1000 Lisboa, Portugal
| | - A Barrau
- Univ. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3, F-38000 Grenoble, France
| | - L Barrin
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
| | | | - L Basara
- INFN TIFPA, I-38123 Povo, Trento, Italy
| | - S Başeğmez-du Pree
- KVI-Center for Advanced Radiation Technology, University of Groningen, NL-9700 AB Groningen, Netherlands
| | - R Battiston
- INFN TIFPA, I-38123 Povo, Trento, Italy
- Università di Trento, I-38123 Povo, Trento, Italy
| | - U Becker
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - M Behlmann
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - B Beischer
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - J Berdugo
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - B Bertucci
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - V Bindi
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - W de Boer
- Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany
| | - K Bollweg
- National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA
| | - B Borgia
- INFN Sezione di Roma 1, I-00185 Roma, Italy
- Università di Roma La Sapienza, I-00185 Roma, Italy
| | - M J Boschini
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
| | - M Bourquin
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - E F Bueno
- Instituto de Física de São Carlos, Universidade de São Paulo, CP 369, 13560-970, São Carlos, São Paulo, SP, Brazil
| | - J Burger
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | | | - X D Cai
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - M Capell
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - S Caroff
- Univ. Grenoble Alpes, Univ. Savoie Mont Blanc, CNRS, LAPP-IN2P3, F-74000 Annecy, France
| | - J Casaus
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | | | - F Cervelli
- INFN Sezione di Pisa, I-56100 Pisa, Italy
| | - Y H Chang
- Physics Department and Center for High Energy and High Field, National Central University (NCU), Tao Yuan, 32054, Taiwan
| | - G M Chen
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - H S Chen
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - Y Chen
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - L Cheng
- Shandong University (SDU), Jinan, Shandong, 250100, China
| | - H Y Chou
- Physics Department and Center for High Energy and High Field, National Central University (NCU), Tao Yuan, 32054, Taiwan
| | - V Choutko
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - C H Chung
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - C Clark
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA
| | - G Coignet
- Univ. Grenoble Alpes, Univ. Savoie Mont Blanc, CNRS, LAPP-IN2P3, F-74000 Annecy, France
| | - C Consolandi
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - A Contin
- INFN Sezione di Bologna, I-40126 Bologna, Italy
- Università di Bologna, I-40126 Bologna, Italy
| | - C Corti
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - M Crispoltoni
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - Z Cui
- Shandong University (SDU), Jinan, Shandong, 250100, China
| | - K Dadzie
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Y M Dai
- Institute of Electrical Engineering (IEE), Chinese Academy of Sciences, Beijing 100190, China
| | - A Datta
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - C Delgado
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - S Della Torre
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
| | - M B Demirköz
- Department of Physics, Middle East Technical University (METU), 06800 Ankara, Turkey
| | - L Derome
- Univ. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3, F-38000 Grenoble, France
| | - S Di Falco
- INFN Sezione di Pisa, I-56100 Pisa, Italy
| | - V Di Felice
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - F Dimiccoli
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
- INFN TIFPA, I-38123 Povo, Trento, Italy
| | - C Díaz
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - P von Doetinchem
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - F Dong
- Southeast University (SEU), Nanjing, 210096, China
| | - F Donnini
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - M Duranti
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - A Egorov
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - A Eline
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - T Eronen
- Space Research Laboratory, Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland
| | - J Feng
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - E Fiandrini
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - P Fisher
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - V Formato
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - Y Galaktionov
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - R J García-López
- Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, and Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
| | - C Gargiulo
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
| | - H Gast
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - I Gebauer
- Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany
| | - M Gervasi
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - F Giovacchini
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - D M Gómez-Coral
- Instituto de Física, Universidad Nacional Autónoma de México (UNAM), México, D. F., 01000 Mexico
| | - J Gong
- Southeast University (SEU), Nanjing, 210096, China
| | - C Goy
- Univ. Grenoble Alpes, Univ. Savoie Mont Blanc, CNRS, LAPP-IN2P3, F-74000 Annecy, France
| | - V Grabski
- Instituto de Física, Universidad Nacional Autónoma de México (UNAM), México, D. F., 01000 Mexico
| | - D Grandi
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - M Graziani
- Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany
| | - K H Guo
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - S Haino
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - K C Han
- National Chung-Shan Institute of Science and Technology (NCSIST), Longtan, Tao Yuan, 32546, Taiwan
| | - Z H He
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - M Heil
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - T H Hsieh
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H Huang
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - Z C Huang
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - M Incagli
- INFN Sezione di Pisa, I-56100 Pisa, Italy
| | - Yi Jia
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H Jinchi
- National Chung-Shan Institute of Science and Technology (NCSIST), Longtan, Tao Yuan, 32546, Taiwan
| | | | - B Khiali
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - Th Kirn
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - C Konak
- Department of Physics, Middle East Technical University (METU), 06800 Ankara, Turkey
| | - O Kounina
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - A Kounine
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - V Koutsenko
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - A Kulemzin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - G La Vacca
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - E Laudi
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
| | - G Laurenti
- INFN Sezione di Bologna, I-40126 Bologna, Italy
| | - I Lazzizzera
- INFN TIFPA, I-38123 Povo, Trento, Italy
- Università di Trento, I-38123 Povo, Trento, Italy
| | - A Lebedev
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H T Lee
- Academia Sinica Grid Center (ASGC), Nankang, Taipei, 11529, Taiwan
| | - S C Lee
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - C Leluc
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - J Q Li
- Southeast University (SEU), Nanjing, 210096, China
| | - Q Li
- Southeast University (SEU), Nanjing, 210096, China
| | - T X Li
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - Z H Li
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - C Light
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - C H Lin
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - T Lippert
- Jülich Supercomputing Centre and JARA-FAME, Research Centre Jülich, D-52425 Jülich, Germany
| | - F Z Liu
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Hu Liu
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- Physics Department and Center for High Energy and High Field, National Central University (NCU), Tao Yuan, 32054, Taiwan
| | - Z Liu
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - S Q Lu
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - Y S Lu
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - K Luebelsmeyer
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - F Luo
- Shandong University (SDU), Jinan, Shandong, 250100, China
| | - J Z Luo
- Southeast University (SEU), Nanjing, 210096, China
| | - Xi Luo
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - S S Lyu
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - F Machate
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - C Mañá
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - J Marín
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - T Martin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA
| | - G Martínez
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - N Masi
- INFN Sezione di Bologna, I-40126 Bologna, Italy
| | - D Maurin
- Univ. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3, F-38000 Grenoble, France
| | - A Menchaca-Rocha
- Instituto de Física, Universidad Nacional Autónoma de México (UNAM), México, D. F., 01000 Mexico
| | - Q Meng
- Southeast University (SEU), Nanjing, 210096, China
| | - D C Mo
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - M Molero
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - P Mott
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA
| | - L Mussolin
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - T Nelson
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - J Q Ni
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - N Nikonov
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - F Nozzoli
- INFN TIFPA, I-38123 Povo, Trento, Italy
| | - A Oliva
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - M Orcinha
- Laboratório de Instrumentação e Física Experimental de Partículas (LIP), P-1000 Lisboa, Portugal
| | - M Palermo
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - F Palmonari
- INFN Sezione di Bologna, I-40126 Bologna, Italy
- Università di Bologna, I-40126 Bologna, Italy
| | - M Paniccia
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - A Pashnin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - M Pauluzzi
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - S Pensotti
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - C Perrina
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - H D Phan
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | | | - V Plyaskin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - M Pohl
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - V Poireau
- Univ. Grenoble Alpes, Univ. Savoie Mont Blanc, CNRS, LAPP-IN2P3, F-74000 Annecy, France
| | - A Popkow
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - L Quadrani
- INFN Sezione di Bologna, I-40126 Bologna, Italy
- Università di Bologna, I-40126 Bologna, Italy
| | - X M Qi
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - X Qin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Z Y Qu
- Institute of Physics, Academia Sinica, Nankang, Taipei, 11529, Taiwan
| | - P G Rancoita
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
| | - D Rapin
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - A Reina Conde
- Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, and Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
| | - S Rosier-Lees
- Univ. Grenoble Alpes, Univ. Savoie Mont Blanc, CNRS, LAPP-IN2P3, F-74000 Annecy, France
| | - A Rozhkov
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - D Rozza
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - R Sagdeev
- East-West Center for Space Science, University of Maryland, College Park, Maryland 20742, USA
| | - C Solano
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - S Schael
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - S M Schmidt
- Jülich Supercomputing Centre and JARA-FAME, Research Centre Jülich, D-52425 Jülich, Germany
| | - A Schulz von Dratzig
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - G Schwering
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - E S Seo
- IPST, University of Maryland, College Park, Maryland 20742, USA
| | - B S Shan
- Beihang University (BUAA), Beijing 100191, China
| | - J Y Shi
- Southeast University (SEU), Nanjing, 210096, China
| | - T Siedenburg
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - J W Song
- Shandong University (SDU), Jinan, Shandong, 250100, China
| | - Z T Sun
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - M Tacconi
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - X W Tang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - Z C Tang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - J Tian
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - Samuel C C Ting
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
| | - S M Ting
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - N Tomassetti
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - J Torsti
- Space Research Laboratory, Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland
| | - T Urban
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- National Aeronautics and Space Administration Johnson Space Center (JSC), Houston, Texas 77058, USA
| | - V Vagelli
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - E Valente
- INFN Sezione di Roma 1, I-00185 Roma, Italy
- Università di Roma La Sapienza, I-00185 Roma, Italy
| | - E Valtonen
- Space Research Laboratory, Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland
| | - M Vázquez Acosta
- Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, and Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
| | - M Vecchi
- KVI-Center for Advanced Radiation Technology, University of Groningen, NL-9700 AB Groningen, Netherlands
- Instituto de Física de São Carlos, Universidade de São Paulo, CP 369, 13560-970, São Carlos, São Paulo, SP, Brazil
| | - M Velasco
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - J P Vialle
- Univ. Grenoble Alpes, Univ. Savoie Mont Blanc, CNRS, LAPP-IN2P3, F-74000 Annecy, France
| | - J Vizán
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - L Q Wang
- Shandong University (SDU), Jinan, Shandong, 250100, China
| | - N H Wang
- Shandong University (SDU), Jinan, Shandong, 250100, China
| | - Q L Wang
- Institute of Electrical Engineering (IEE), Chinese Academy of Sciences, Beijing 100190, China
| | - X Wang
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - X Q Wang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - Z X Wang
- Sun Yat-Sen University (SYSU), Guangzhou, 510275, China
| | - J Wei
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - Z L Weng
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H Wu
- Southeast University (SEU), Nanjing, 210096, China
| | - R Q Xiong
- Southeast University (SEU), Nanjing, 210096, China
| | - W Xu
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Q Yan
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Y Yang
- National Cheng Kung University, Tainan, 70101, Taiwan
| | - H Yi
- Southeast University (SEU), Nanjing, 210096, China
| | - Y J Yu
- Institute of Electrical Engineering (IEE), Chinese Academy of Sciences, Beijing 100190, China
| | - Z Q Yu
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - M Zannoni
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - S Zeissler
- Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany
| | - C Zhang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - F Zhang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - J H Zhang
- Southeast University (SEU), Nanjing, 210096, China
| | - Z Zhang
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - F Zhao
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - Z M Zheng
- Beihang University (BUAA), Beijing 100191, China
| | - H L Zhuang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - V Zhukov
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - A Zichichi
- INFN Sezione di Bologna, I-40126 Bologna, Italy
- Università di Bologna, I-40126 Bologna, Italy
| | - N Zimmermann
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - P Zuccon
- INFN TIFPA, I-38123 Povo, Trento, Italy
- Università di Trento, I-38123 Povo, Trento, Italy
| |
Collapse
|
13
|
Aguilar M, Ali Cavasonza L, Ambrosi G, Arruda L, Attig N, Azzarello P, Bachlechner A, Barao F, Barrau A, Barrin L, Bartoloni A, Basara L, Başeğmez-du Pree S, Battiston R, Becker U, Behlmann M, Beischer B, Berdugo J, Bertucci B, Bindi V, de Boer W, Bollweg K, Borgia B, Boschini MJ, Bourquin M, Bueno EF, Burger J, Burger WJ, Cai XD, Capell M, Caroff S, Casaus J, Castellini G, Cervelli F, Chang YH, Chen GM, Chen HS, Chen Y, Cheng L, Chou HY, Choutko V, Chung CH, Clark C, Coignet G, Consolandi C, Contin A, Corti C, Crispoltoni M, Cui Z, Dadzie K, Dai YM, Datta A, Delgado C, Della Torre S, Demirköz MB, Derome L, Di Falco S, Dimiccoli F, Díaz C, von Doetinchem P, Dong F, Donnini F, Duranti M, Egorov A, Eline A, Eronen T, Feng J, Fiandrini E, Fisher P, Formato V, Galaktionov Y, García-López RJ, Gargiulo C, Gast H, Gebauer I, Gervasi M, Giovacchini F, Gómez-Coral DM, Gong J, Goy C, Grabski V, Grandi D, Graziani M, Guo KH, Haino S, Han KC, He ZH, Heil M, Hsieh TH, Huang H, Huang ZC, Incagli M, Jia Y, Jinchi H, Kanishev K, Khiali B, Kirn T, Konak C, Kounina O, Kounine A, Koutsenko V, Kulemzin A, La Vacca G, Laudi E, Laurenti G, Lazzizzera I, Lebedev A, Lee HT, Lee SC, Leluc C, Li JQ, Li Q, Li TX, Li ZH, Light C, Lin CH, Lippert T, Liu FZ, Liu H, Liu Z, Lu SQ, Lu YS, Luebelsmeyer K, Luo F, Luo JZ, Luo X, Lyu SS, Machate F, Mañá C, Marín J, Martin T, Martínez G, Masi N, Maurin D, Menchaca-Rocha A, Meng Q, Mo DC, Molero M, Mott P, Mussolin L, Nelson T, Ni JQ, Nikonov N, Nozzoli F, Oliva A, Orcinha M, Palermo M, Palmonari F, Paniccia M, Pashnin A, Pauluzzi M, Pensotti S, Perrina C, Phan HD, Picot-Clemente N, Plyaskin V, Pohl M, Poireau V, Popkow A, Quadrani L, Qi XM, Qin X, Qu ZY, Rancoita PG, Rapin D, Conde AR, Rosier-Lees S, Rozhkov A, Rozza D, Sagdeev R, Solano C, Schael S, Schmidt SM, Schulz von Dratzig A, Schwering G, Seo ES, Shan BS, Shi JY, Siedenburg T, Song JW, Sun ZT, Tacconi M, Tang XW, Tang ZC, Tian J, Ting SCC, Ting SM, Tomassetti N, Torsti J, Urban T, Vagelli V, Valente E, Valtonen E, Vázquez Acosta M, Vecchi M, Velasco M, Vialle JP, Vizán J, Wang LQ, Wang NH, Wang QL, Wang X, Wang XQ, Wang ZX, Wei J, Weng ZL, Wu H, Xiong RQ, Xu W, Yan Q, Yang Y, Yi H, Yu YJ, Yu ZQ, Zannoni M, Zeissler S, Zhang C, Zhang F, Zhang JH, Zhang Z, Zhao F, Zheng ZM, Zhuang HL, Zhukov V, Zichichi A, Zimmermann N, Zuccon P. Towards Understanding the Origin of Cosmic-Ray Positrons. Phys Rev Lett 2019; 122:041102. [PMID: 30768313 DOI: 10.1103/physrevlett.122.041102] [Citation(s) in RCA: 32] [Impact Index Per Article: 6.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/21/2018] [Revised: 12/04/2018] [Indexed: 06/09/2023]
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 E_{s}=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.
Collapse
Affiliation(s)
- M Aguilar
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - L Ali Cavasonza
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - G Ambrosi
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - L Arruda
- Laboratório de Instrumentação e Física Experimental de Partículas (LIP), P-1000 Lisboa, Portugal
| | - N Attig
- Jülich Supercomputing Centre and JARA-FAME, Research Centre Jülich, D-52425 Jülich, Germany
| | - P Azzarello
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - A Bachlechner
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - F Barao
- Laboratório de Instrumentação e Física Experimental de Partículas (LIP), P-1000 Lisboa, Portugal
| | - A Barrau
- Univ. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3, F-38000 Grenoble, France
| | - L Barrin
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
| | | | - L Basara
- INFN TIFPA, I-38123 Povo, Trento, Italy
| | - S Başeğmez-du Pree
- KVI-Center for Advanced Radiation Technology, University of Groningen, NL-9700 AB Groningen, the Netherlands
| | - R Battiston
- INFN TIFPA, I-38123 Povo, Trento, Italy
- Università di Trento, I-38123 Povo, Trento, Italy
| | - U Becker
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - M Behlmann
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - B Beischer
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - J Berdugo
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - B Bertucci
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - V Bindi
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - W de Boer
- Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany
| | - K Bollweg
- National Aeronautics and Space Administration Johnson Space Center (JSC), Jacobs Engineering, and Business Integra, Houston, Texas 77058, USA
| | - B Borgia
- INFN Sezione di Roma 1, I-00185 Roma, Italy
- Università di Roma La Sapienza, I-00185 Roma, Italy
| | - M J Boschini
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
| | - M Bourquin
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - E F Bueno
- Instituto de Física de São Carlos, Universidade de São Paulo, CP 369, 13560-970 São Carlos, São Paulo, SP, Brazil
| | - J Burger
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | | | - X D Cai
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - M Capell
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - S Caroff
- Université Grenoble Alpes, Université Savoie Mont Blanc, CNRS, LAPP-IN2P3, F-74000 Annecy, France
| | - J Casaus
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | | | - F Cervelli
- INFN Sezione di Pisa, I-56100 Pisa, Italy
| | - Y H Chang
- Physics Department and Center for High Energy and High Field, National Central University (NCU), Tao Yuan 32054, Taiwan
| | - G M Chen
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - H S Chen
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - Y Chen
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - L Cheng
- Shandong University (SDU), Jinan, Shandong 250100, China
| | - H Y Chou
- Physics Department and Center for High Energy and High Field, National Central University (NCU), Tao Yuan 32054, Taiwan
| | - V Choutko
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - C H Chung
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - C Clark
- National Aeronautics and Space Administration Johnson Space Center (JSC), Jacobs Engineering, and Business Integra, Houston, Texas 77058, USA
| | - G Coignet
- Université Grenoble Alpes, Université Savoie Mont Blanc, CNRS, LAPP-IN2P3, F-74000 Annecy, France
| | - C Consolandi
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - A Contin
- INFN Sezione di Bologna, I-40126 Bologna, Italy
- Università di Bologna, I-40126 Bologna, Italy
| | - C Corti
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - M Crispoltoni
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - Z Cui
- Shandong University (SDU), Jinan, Shandong 250100, China
| | - K Dadzie
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Y M Dai
- Institute of Electrical Engineering (IEE), Chinese Academy of Sciences, Beijing 100190, China
| | - A Datta
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - C Delgado
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - S Della Torre
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
| | - M B Demirköz
- Department of Physics, Middle East Technical University (METU), 06800 Ankara, Turkey
| | - L Derome
- Univ. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3, F-38000 Grenoble, France
| | - S Di Falco
- INFN Sezione di Pisa, I-56100 Pisa, Italy
| | - F Dimiccoli
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
- INFN TIFPA, I-38123 Povo, Trento, Italy
| | - C Díaz
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - P von Doetinchem
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - F Dong
- Southeast University (SEU), Nanjing 210096, China
| | - F Donnini
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - M Duranti
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - A Egorov
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - A Eline
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - T Eronen
- Space Research Laboratory, Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland
| | - J Feng
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - E Fiandrini
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - P Fisher
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - V Formato
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - Y Galaktionov
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - R J García-López
- Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, and Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
| | - C Gargiulo
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
| | - H Gast
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - I Gebauer
- Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany
| | - M Gervasi
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - F Giovacchini
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - D M Gómez-Coral
- Instituto de Física, Universidad Nacional Autónoma de México (UNAM), México, D. F., 01000 Mexico
| | - J Gong
- Southeast University (SEU), Nanjing 210096, China
| | - C Goy
- Université Grenoble Alpes, Université Savoie Mont Blanc, CNRS, LAPP-IN2P3, F-74000 Annecy, France
| | - V Grabski
- Instituto de Física, Universidad Nacional Autónoma de México (UNAM), México, D. F., 01000 Mexico
| | - D Grandi
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - M Graziani
- Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany
| | - K H Guo
- Sun Yat-Sen University (SYSU), Guangzhou 510275, China
| | - S Haino
- Institute of Physics, Academia Sinica, Nankang, Taipei 11529, Taiwan
| | - K C Han
- National Chung-Shan Institute of Science and Technology (NCSIST), Longtan, Tao Yuan 32546, Taiwan
| | - Z H He
- Sun Yat-Sen University (SYSU), Guangzhou 510275, China
| | - M Heil
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - T H Hsieh
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H Huang
- Institute of Physics, Academia Sinica, Nankang, Taipei 11529, Taiwan
| | - Z C Huang
- Sun Yat-Sen University (SYSU), Guangzhou 510275, China
| | - M Incagli
- INFN Sezione di Pisa, I-56100 Pisa, Italy
| | - Yi Jia
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H Jinchi
- National Chung-Shan Institute of Science and Technology (NCSIST), Longtan, Tao Yuan 32546, Taiwan
| | | | - B Khiali
- INFN Sezione di Perugia, I-06100 Perugia, Italy
| | - Th Kirn
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - C Konak
- Department of Physics, Middle East Technical University (METU), 06800 Ankara, Turkey
| | - O Kounina
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - A Kounine
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - V Koutsenko
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - A Kulemzin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - G La Vacca
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - E Laudi
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
| | - G Laurenti
- INFN Sezione di Bologna, I-40126 Bologna, Italy
| | - I Lazzizzera
- INFN TIFPA, I-38123 Povo, Trento, Italy
- Università di Trento, I-38123 Povo, Trento, Italy
| | - A Lebedev
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H T Lee
- Academia Sinica Grid Center (ASGC), Nankang, Taipei 11529, Taiwan
| | - S C Lee
- Institute of Physics, Academia Sinica, Nankang, Taipei 11529, Taiwan
| | - C Leluc
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - J Q Li
- Southeast University (SEU), Nanjing 210096, China
| | - Q Li
- Southeast University (SEU), Nanjing 210096, China
| | - T X Li
- Sun Yat-Sen University (SYSU), Guangzhou 510275, China
| | - Z H Li
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - C Light
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - C H Lin
- Institute of Physics, Academia Sinica, Nankang, Taipei 11529, Taiwan
| | - T Lippert
- Jülich Supercomputing Centre and JARA-FAME, Research Centre Jülich, D-52425 Jülich, Germany
| | - F Z Liu
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Hu Liu
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- Physics Department and Center for High Energy and High Field, National Central University (NCU), Tao Yuan 32054, Taiwan
| | - Z Liu
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - S Q Lu
- Institute of Physics, Academia Sinica, Nankang, Taipei 11529, Taiwan
| | - Y S Lu
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - K Luebelsmeyer
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - F Luo
- Shandong University (SDU), Jinan, Shandong 250100, China
| | - J Z Luo
- Southeast University (SEU), Nanjing 210096, China
| | - Xi Luo
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - S S Lyu
- Sun Yat-Sen University (SYSU), Guangzhou 510275, China
| | - F Machate
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - C Mañá
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - J Marín
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - T Martin
- National Aeronautics and Space Administration Johnson Space Center (JSC), Jacobs Engineering, and Business Integra, Houston, Texas 77058, USA
| | - G Martínez
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - N Masi
- INFN Sezione di Bologna, I-40126 Bologna, Italy
| | - D Maurin
- Univ. Grenoble Alpes, CNRS, Grenoble INP, LPSC-IN2P3, F-38000 Grenoble, France
| | - A Menchaca-Rocha
- Instituto de Física, Universidad Nacional Autónoma de México (UNAM), México, D. F., 01000 Mexico
| | - Q Meng
- Southeast University (SEU), Nanjing 210096, China
| | - D C Mo
- Sun Yat-Sen University (SYSU), Guangzhou 510275, China
| | - M Molero
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - P Mott
- National Aeronautics and Space Administration Johnson Space Center (JSC), Jacobs Engineering, and Business Integra, Houston, Texas 77058, USA
| | - L Mussolin
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - T Nelson
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - J Q Ni
- Sun Yat-Sen University (SYSU), Guangzhou 510275, China
| | - N Nikonov
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - F Nozzoli
- INFN TIFPA, I-38123 Povo, Trento, Italy
| | - A Oliva
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - M Orcinha
- Laboratório de Instrumentação e Física Experimental de Partículas (LIP), P-1000 Lisboa, Portugal
| | - M Palermo
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - F Palmonari
- INFN Sezione di Bologna, I-40126 Bologna, Italy
- Università di Bologna, I-40126 Bologna, Italy
| | - M Paniccia
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - A Pashnin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - M Pauluzzi
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - S Pensotti
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - C Perrina
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - H D Phan
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | | | - V Plyaskin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - M Pohl
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - V Poireau
- Université Grenoble Alpes, Université Savoie Mont Blanc, CNRS, LAPP-IN2P3, F-74000 Annecy, France
| | - A Popkow
- Physics and Astronomy Department, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - L Quadrani
- INFN Sezione di Bologna, I-40126 Bologna, Italy
- Università di Bologna, I-40126 Bologna, Italy
| | - X M Qi
- Sun Yat-Sen University (SYSU), Guangzhou 510275, China
| | - X Qin
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Z Y Qu
- Institute of Physics, Academia Sinica, Nankang, Taipei 11529, Taiwan
| | - P G Rancoita
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
| | - D Rapin
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - A Reina Conde
- Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, and Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
| | - S Rosier-Lees
- Université Grenoble Alpes, Université Savoie Mont Blanc, CNRS, LAPP-IN2P3, F-74000 Annecy, France
| | - A Rozhkov
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - D Rozza
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - R Sagdeev
- East-West Center for Space Science, University of Maryland, College Park, Maryland 20742, USA
| | - C Solano
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - S Schael
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - S M Schmidt
- Jülich Supercomputing Centre and JARA-FAME, Research Centre Jülich, D-52425 Jülich, Germany
| | - A Schulz von Dratzig
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - G Schwering
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - E S Seo
- IPST, University of Maryland, College Park, Maryland 20742, USA
| | - B S Shan
- Beihang University (BUAA), Beijing 100191, China
| | - J Y Shi
- Southeast University (SEU), Nanjing 210096, China
| | - T Siedenburg
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - J W Song
- Shandong University (SDU), Jinan, Shandong 250100, China
| | - Z T Sun
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - M Tacconi
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - X W Tang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - Z C Tang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - J Tian
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - Samuel C C Ting
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
- European Organization for Nuclear Research (CERN), CH-1211 Geneva 23, Switzerland
| | - S M Ting
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - N Tomassetti
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - J Torsti
- Space Research Laboratory, Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland
| | - T Urban
- National Aeronautics and Space Administration Johnson Space Center (JSC), Jacobs Engineering, and Business Integra, Houston, Texas 77058, USA
| | - V Vagelli
- INFN Sezione di Perugia, I-06100 Perugia, Italy
- Università di Perugia, I-06100 Perugia, Italy
| | - E Valente
- INFN Sezione di Roma 1, I-00185 Roma, Italy
- Università di Roma La Sapienza, I-00185 Roma, Italy
| | - E Valtonen
- Space Research Laboratory, Department of Physics and Astronomy, University of Turku, FI-20014 Turku, Finland
| | - M Vázquez Acosta
- Instituto de Astrofísica de Canarias (IAC), E-38205 La Laguna, and Departamento de Astrofísica, Universidad de La Laguna, E-38206 La Laguna, Tenerife, Spain
| | - M Vecchi
- KVI-Center for Advanced Radiation Technology, University of Groningen, NL-9700 AB Groningen, the Netherlands
- Instituto de Física de São Carlos, Universidade de São Paulo, CP 369, 13560-970 São Carlos, São Paulo, SP, Brazil
| | - M Velasco
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - J P Vialle
- Université Grenoble Alpes, Université Savoie Mont Blanc, CNRS, LAPP-IN2P3, F-74000 Annecy, France
| | - J Vizán
- Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas (CIEMAT), E-28040 Madrid, Spain
| | - L Q Wang
- Shandong University (SDU), Jinan, Shandong 250100, China
| | - N H Wang
- Shandong University (SDU), Jinan, Shandong 250100, China
| | - Q L Wang
- Institute of Electrical Engineering (IEE), Chinese Academy of Sciences, Beijing 100190, China
| | - X Wang
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - X Q Wang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - Z X Wang
- Sun Yat-Sen University (SYSU), Guangzhou 510275, China
| | - J Wei
- DPNC, Université de Genève, CH-1211 Genève 4, Switzerland
| | - Z L Weng
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - H Wu
- Southeast University (SEU), Nanjing 210096, China
| | - R Q Xiong
- Southeast University (SEU), Nanjing 210096, China
| | - W Xu
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Q Yan
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - Y Yang
- National Cheng Kung University, Tainan 70101, Taiwan
| | - H Yi
- Southeast University (SEU), Nanjing 210096, China
| | - Y J Yu
- Institute of Electrical Engineering (IEE), Chinese Academy of Sciences, Beijing 100190, China
| | - Z Q Yu
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - M Zannoni
- INFN Sezione di Milano-Bicocca, I-20126 Milano, Italy
- Università di Milano-Bicocca, I-20126 Milano, Italy
| | - S Zeissler
- Institut für Experimentelle Teilchenphysik, Karlsruhe Institute of Technology (KIT), D-76131 Karlsruhe, Germany
| | - C Zhang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - F Zhang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - J H Zhang
- Southeast University (SEU), Nanjing 210096, China
| | - Z Zhang
- Massachusetts Institute of Technology (MIT), Cambridge, Massachusetts 02139, USA
| | - F Zhao
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
- University of Chinese Academy of Sciences (UCAS), Beijing 100049, China
| | - Z M Zheng
- Beihang University (BUAA), Beijing 100191, China
| | - H L Zhuang
- Institute of High Energy Physics (IHEP), Chinese Academy of Sciences, Beijing 100049, China
| | - V Zhukov
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - A Zichichi
- INFN Sezione di Bologna, I-40126 Bologna, Italy
- Università di Bologna, I-40126 Bologna, Italy
| | - N Zimmermann
- I. Physics Institute and JARA-FAME, RWTH Aachen University, D-52056 Aachen, Germany
| | - P Zuccon
- INFN TIFPA, I-38123 Povo, Trento, Italy
- Università di Trento, I-38123 Povo, Trento, Italy
| |
Collapse
|
14
|
Nozzoli F. Properties of Elementary Particle Fluxes in Primary Cosmic Rays Measured with the Alpha Magnetic Spectrometer on the International Space Station. EPJ Web Conf 2019. [DOI: 10.1051/epjconf/201920901007] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/15/2022] Open
Abstract
Precision measurements by AMS of the fluxes of cosmic ray positrons, electrons, antiprotons, protons as well as their rations reveal several unexpected and intriguing features. The presented measurements extend the energy range of the previous observations with much increased precision. The new results show that the behavior of positron flux at around 300 GeV is consistent with a new source that produce equal amount of high energy electrons and positrons. In addition, in the absolute rigidity range 60–500 GV, the antiproton, proton, and positron fluxes are found to have nearly identical rigidity dependence and the electron flux exhibits different rigidity dependence.
Collapse
|
15
|
Abstract
There is a commonly expressed opinion in the literature, that cosmic-ray (CR) e+ come from a primary source, which could be dark matter or pulsars. In these proceedings we review some evidence to the contrary: namely, that e+ come from secondary production due to CR nuclei scattering on interstellar matter. We show that recent measurements of the total e± flux at E ≲ 3 TeV are in good agreement with the predicted flux of secondary e±, that would be obtained if radiative energy losses during CR propagation do not play an important role. If the agreement between data and secondary prediction is not accidental, then the requirement of negligible radiative energy losses implies a very short propagation time for high energy CRs: tesc ≲. 105 yr at rigidities R ≳ 3 TV. Such short propagation history may imply that a recent, near-by source dominates the CRs at these energies. We review independent evidence for a transition in CR propagation, based on the spectral hardening of primary and secondary nuclei around R ~ 100 GV. The transition rigidity of the nuclei matches the rigidity at which the e+ flux saturates its secondary upper bound.
Collapse
|
16
|
Abstract
DAMPE (DArk Matter Particle Explorer) is a satellite-born experiment, resulting from the collaboration of Chinese, Italian, and Swiss institutions. Since December 2015, DAMPE flights at the altitude of 500 km and collects data smoothly. The detector is made of four sub-detectors: top layers of plastic scintillators, a silicon-tungsten tracker, a BGO calorimeter (32 radiation lengths), and a bottom boron-doped scintillator to detect delayed neutrons. The main goal of the experiment is the search for indirect signals of Dark Matter in the electron and photon spectra with energies up to 10 TeV. Furthermore DAMPE studies cosmic charged and gamma radiation. The calorimeter depth and the large acceptance allow to measure cosmic ray fluxes in the range from 20 GeV up to hundreds of TeV. An overview of the latest results about light component (p+He) of charged cosmic rays, gamma astronomy and electron and positron spectrum will be presented.
Collapse
|
17
|
Asaoka Y, Adriani O, Akaike Y, Asano K, Bagliesi MG, Berti E, Bigongiari G, Binns WR, Bonechi S, Bongi M, Bruno A, Brogi P, Buckley JH, Cannady N, Castellini G, Checchia C, Cherry ML, Collazuol G, Di Felice V, Ebisawa K, Fuke H, Guzik TG, Hams T, Hasebe N, Hibinov K, Ichimura M, Ioka K, Ishizaki W, Israel MH, Kasahara K, Kataoka J, Kataoka R, Katayose Y, Kato C, Kawanaka N, Kawakubo Y, Kohri K, Krawczynski HS, Krizmanic JF, Lomtadze T, Maestro P, Marrocchesi PS, Messineo AM, Mitchell JW, Miyake S, Moiseev AA, Mori K, Mori M, Mori N, Motz HM, Munakata K, Murakami H, Nakahira S, Nishimura J, De Nolfo GA, Okuno S, Ormes JF, Ozawa S, Pacini L, Palma F, Pal'shin V, Papini P, Penacchioni AV, Rauch BF, Ricciarini SB, Sakai K, Sakamoto T, Sasaki M, Shimizu Y, Shiomi A, Sparvoli R, Spillantini P, Stolzi F, Sugita S, Suh JE, Sulaj A, Takahashi I, Takayanagi M, Takita M, Tamura T, Tateyama N, Terasawa T, Tomida H, Torii S, Tsunesada Y, Uchihori Y, Ueno S, Vannuccini E, Wefel JP, Yamaoka K, Yanagita S, Yoshida A, Yoshida K. The CALorimetric Electron Telescope (CALET) on the International Space Station: Results from the First Two Years of Operation. EPJ Web Conf 2019. [DOI: 10.1051/epjconf/201920813001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
The CALorimetric Electron Telescope (CALET) space experiment, which has been developed by Japan in collaboration with Italy and the United States, is a high-energy astroparticle physics mission on the International Space Station (ISS). The primary goals of the CALET mission include investigation of possible nearby sources of high-energy electrons, detailed study of galactic cosmic-ray acceleration and propagation, and search for dark matter signatures. With a long-term observation onboard the ISS, the CALET experiment measures the flux of cosmic-ray electrons (including positrons) up to 20 TeV, gamma-rays to 10 TeV, and nuclei up to 1,000 TeV based on its charge separation capability from Z = 1 to 40. Since the start of science operation in mid-October, 2015, a continuous observation has been maintained without any major interruptions. The number of triggered events over 10 GeV is nearly 20 million per month. By using the data obtained during the first two-years, here we present a summary of the CALET observations: 1) Electron+positron energy spectrum, 2) Nuclei analysis, 3) Gamma-ray observation with a characterization of the on-orbit performance. The search results for the electromagnetic counterparts of LIGO/Virgo gravitational wave events are also discussed.
Collapse
|
18
|
de Naurois M. Highlights from H.E.S.S. EPJ Web Conf 2019. [DOI: 10.1051/epjconf/201920901025] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
In the 15 years since its construction, the H.E.S.S. gamma-ray observatory has allowed the study of the Very High Energy gamma-ray sky at resolutions and sensitivities which were never before possible. During this period H.E.S.S. has discovered a rich zoo of both galactic and extra galactic source classes, made measurements of the galactic cosmic ray spectrum and placed limits on fundamental physical processes. A summary of the latest H.E.S.S. results for these source classes has been presented at the conference, describing the most interesting new observations and their physical interpretation. Additionally the latest upgrades and improvements to the H.E.S.S. hardware and data analyses, and the future science prospects for the experiment have been described.
Collapse
|
19
|
Abstract
The Alpha Magnetic Spectrometer, AMS-02, detector is operating on the International Space Station (ISS) since May the 19th, 2011. More than 120 billion events have been collected by the instrument in the first 7 years of data taking, providing detailed insight on the features of different species of cosmic rays. This contribution reviews the recent AMS-02 results based on 7 years of operations in space and their contribution to the advances in the understanding of cosmic ray origin, acceleration and propagation physics.
Collapse
|
20
|
Jin HB, Yue B, Zhang X, Chen X. Dark matter explanation of the cosmic ray
e+e−
spectrum excess and peak feature observed by the DAMPE experiment. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.98.123008] [Citation(s) in RCA: 8] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
21
|
Archer A, Benbow W, Bird R, Brose R, Buchovecky M, Buckley J, Bugaev V, Connolly M, Cui W, Daniel M, Feng Q, Finley J, Fortson L, Furniss A, Gillanders G, Hütten M, Hanna D, Hervet O, Holder J, Hughes G, Humensky T, Johnson C, Kaaret P, Kar P, Kelley-Hoskins N, Kertzman M, Kieda D, Krause M, Krennrich F, Kumar S, Lang M, Lin T, Maier G, McArthur S, Moriarty P, Mukherjee R, O’Brien S, Ong R, Otte A, Petrashyk A, Pohl M, Pueschel E, Quinn J, Ragan K, Reynolds P, Richards G, Roache E, Rulten C, Sadeh I, Santander M, Sembroski G, Staszak D, Sushch I, Wakely S, Wells R, Wilcox P, Wilhelm A, Williams D, Williamson T, Zitzer B. Measurement of cosmic-ray electrons at TeV energies by VERITAS. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.98.062004] [Citation(s) in RCA: 20] [Impact Index Per Article: 3.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
22
|
|
23
|
Mazziotta M, Costanza F, Cuoco A, Gargano F, Loparco F, Zimmer S. Search for features in the cosmic-ray electron and positron spectrum measured by the Fermi Large Area Telescope. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.98.022006] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
24
|
Adriani O, Akaike Y, Asano K, Asaoka Y, Bagliesi MG, Berti E, Bigongiari G, Binns WR, Bonechi S, Bongi M, Brogi P, Buckley JH, Cannady N, Castellini G, Checchia C, Cherry ML, Collazuol G, Di Felice V, Ebisawa K, Fuke H, Guzik TG, Hams T, Hareyama M, Hasebe N, Hibino K, Ichimura M, Ioka K, Ishizaki W, Israel MH, Kasahara K, Kataoka J, Kataoka R, Katayose Y, Kato C, Kawanaka N, Kawakubo Y, Kohri K, Krawczynski HS, Krizmanic JF, Lomtadze T, Maestro P, Marrocchesi PS, Messineo AM, Mitchell JW, Miyake S, Moiseev AA, Mori K, Mori M, Mori N, Motz HM, Munakata K, Murakami H, Nakahira S, Nishimura J, de Nolfo GA, Okuno S, Ormes JF, Ozawa S, Pacini L, Palma F, Papini P, Penacchioni AV, Rauch BF, Ricciarini SB, Sakai K, Sakamoto T, Sasaki M, Shimizu Y, Shiomi A, Sparvoli R, Spillantini P, Stolzi F, Suh JE, Sulaj A, Takahashi I, Takayanagi M, Takita M, Tamura T, Tateyama N, Terasawa T, Tomida H, Torii S, Tsunesada Y, Uchihori Y, Ueno S, Vannuccini E, Wefel JP, Yamaoka K, Yanagita S, Yoshida A, Yoshida K. Extended Measurement of the Cosmic-Ray Electron and Positron Spectrum from 11 GeV to 4.8 TeV with the Calorimetric Electron Telescope on the International Space Station. Phys Rev Lett 2018; 120:261102. [PMID: 30004739 DOI: 10.1103/physrevlett.120.261102] [Citation(s) in RCA: 13] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/16/2018] [Revised: 05/21/2018] [Indexed: 06/08/2023]
Abstract
Extended results on the cosmic-ray electron + positron spectrum from 11 GeV to 4.8 TeV are presented based on observations with the Calorimetric Electron Telescope (CALET) on the International Space Station utilizing the data up to November 2017. The analysis uses the full detector acceptance at high energies, approximately doubling the statistics compared to the previous result. CALET is an all-calorimetric instrument with a total thickness of 30 X_{0} at normal incidence and fine imaging capability, designed to achieve large proton rejection and excellent energy resolution well into the TeV energy region. The observed energy spectrum in the region below 1 TeV shows good agreement with Alpha Magnetic Spectrometer (AMS-02) data. In the energy region below ∼300 GeV, CALET's spectral index is found to be consistent with the AMS-02, Fermi Large Area Telescope (Fermi-LAT), and Dark Matter Particle Explorer (DAMPE), while from 300 to 600 GeV the spectrum is significantly softer than the spectra from the latter two experiments. The absolute flux of CALET is consistent with other experiments at around a few tens of GeV. However, it is lower than those of DAMPE and Fermi-LAT with the difference increasing up to several hundred GeV. The observed energy spectrum above ∼1 TeV suggests a flux suppression consistent within the errors with the results of DAMPE, while CALET does not observe any significant evidence for a narrow spectral feature in the energy region around 1.4 TeV. Our measured all-electron flux, including statistical errors and a detailed breakdown of the systematic errors, is tabulated in the Supplemental Material in order to allow more refined spectral analyses based on our data.
Collapse
Affiliation(s)
- O Adriani
- Department of Physics, University of Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - Y Akaike
- Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - K Asano
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - Y Asaoka
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
- JEM Utilization Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
| | - M G Bagliesi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - E Berti
- Department of Physics, University of Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - G Bigongiari
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - W R Binns
- Department of Physics, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - S Bonechi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - M Bongi
- Department of Physics, University of Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - P Brogi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - J H Buckley
- Department of Physics, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - N Cannady
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - G Castellini
- Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 50019 Sesto, Fiorentino, Italy
| | - C Checchia
- Department of Physics and Astronomy, University of Padova, Via Marzolo, 8, 35131 Padova, Italy
- INFN Sezione di Padova, Via Marzolo, 8, 35131 Padova, Italy
| | - M L Cherry
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - G Collazuol
- Department of Physics and Astronomy, University of Padova, Via Marzolo, 8, 35131 Padova, Italy
- INFN Sezione di Padova, Via Marzolo, 8, 35131 Padova, Italy
| | - V Di Felice
- University of Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
- INFN Sezione di Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
| | - K Ebisawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - H Fuke
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - T G Guzik
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - T Hams
- Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - M Hareyama
- St. Marianna University School of Medicine, 2-16-1, Sugao, Miyamae-ku, Kawasaki, Kanagawa 216-8511, Japan
| | - N Hasebe
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - K Hibino
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - M Ichimura
- Faculty of Science and Technology, Graduate School of Science and Technology, Hirosaki University, 3, Bunkyo, Hirosaki, Aomori 036-8561, Japan
| | - K Ioka
- Yukawa Institute for Theoretical Physics, Kyoto University, Kitashirakawa Oiwakecho, Sakyo, Kyoto 606-8502, Japan
| | - W Ishizaki
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - M H Israel
- Department of Physics, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - K Kasahara
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - J Kataoka
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - R Kataoka
- National Institute of Polar Research, 10-3, Midori-cho, Tachikawa, Tokyo 190-8518, Japan
| | - Y Katayose
- Faculty of Engineering, Division of Intelligent Systems Engineering, Yokohama National University, 79-5 Tokiwadai, Hodogaya, Yokohama 240-8501, Japan
| | - C Kato
- Faculty of Science, Shinshu University, 3-1-1 Asahi, Matsumoto, Nagano 390-8621, Japan
| | - N Kawanaka
- Hakubi Center, Kyoto University, Yoshida Honmachi, Sakyo-ku, Kyoto 606-8501, Japan
- Department of Astronomy, Graduate School of Science, Kyoto University, Kitashirakawa Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
| | - Y Kawakubo
- College of Science and Engineering, Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo, Sagamihara, Kanagawa 252-5258, Japan
| | - K Kohri
- Institute of Particle and Nuclear Studies, High Energy Accelerator Research Organization, 1-1 Oho, Tsukuba, Ibaraki 305-0801, Japan
| | - H S Krawczynski
- Department of Physics, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - J F Krizmanic
- Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - T Lomtadze
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - P Maestro
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - P S Marrocchesi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - A M Messineo
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
- University of Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - J W Mitchell
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - S Miyake
- Department of Electrical and Electronic Systems Engineering, National Institute of Technology, Ibaraki College, 866 Nakane, Hitachinaka, Ibaraki 312-8508 Japan
| | - A A Moiseev
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
- Department of Astronomy, University of Maryland, College Park, Maryland 20742, USA
| | - K Mori
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - M Mori
- Department of Physical Sciences, College of Science and Engineering, Ritsumeikan University, Shiga 525-8577, Japan
| | - N Mori
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - H M Motz
- International Center for Science and Engineering Programs, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - K Munakata
- Faculty of Science, Shinshu University, 3-1-1 Asahi, Matsumoto, Nagano 390-8621, Japan
| | - H Murakami
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - S Nakahira
- RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan
| | - J Nishimura
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - G A de Nolfo
- Heliospheric Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - S Okuno
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - J F Ormes
- Department of Physics and Astronomy, University of Denver, Physics Building, Room 211, 2112 East Wesley Avenue, Denver, Colorado 80208-6900, USA
| | - S Ozawa
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - L Pacini
- Department of Physics, University of Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
- Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 50019 Sesto, Fiorentino, Italy
| | - F Palma
- University of Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
- INFN Sezione di Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
| | - P Papini
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - A V Penacchioni
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- ASI Science Data Center (ASDC), Via del Politecnico snc, 00133 Rome, Italy
| | - B F Rauch
- Department of Physics, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - S B Ricciarini
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
- Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 50019 Sesto, Fiorentino, Italy
| | - K Sakai
- Department of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - T Sakamoto
- College of Science and Engineering, Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo, Sagamihara, Kanagawa 252-5258, Japan
| | - M Sasaki
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
- Department of Astronomy, University of Maryland, College Park, Maryland 20742, USA
| | - Y Shimizu
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - A Shiomi
- College of Industrial Technology, Nihon University, 1-2-1 Izumi, Narashino, Chiba 275-8575, Japan
| | - R Sparvoli
- University of Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
- INFN Sezione di Rome "Tor Vergata", Via della Ricerca Scientifica 1, 00133 Rome, Italy
| | - P Spillantini
- Department of Physics, University of Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - F Stolzi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - J E Suh
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - A Sulaj
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - I Takahashi
- Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, 277-8583, Japan
| | - M Takayanagi
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - M Takita
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - T Tamura
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - N Tateyama
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - T Terasawa
- RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan
| | - H Tomida
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - S Torii
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
- JEM Utilization Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- School of Advanced Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - Y Tsunesada
- Division of Mathematics and Physics, Graduate School of Science, Osaka City University, 3-3-138 Sugimoto, Sumiyoshi, Osaka 558-8585, Japan
| | - Y Uchihori
- National Institutes for Quantum and Radiation Science and Technology, 4-9-1 Anagawa, Inage, Chiba 263-8555, Japan
| | - S Ueno
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - E Vannuccini
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - J P Wefel
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - K Yamaoka
- Nagoya University, Furo, Chikusa, Nagoya 464-8601, Japan
| | - S Yanagita
- College of Science, Ibaraki University, 2-1-1 Bunkyo, Mito, Ibaraki 310-8512, Japan
| | - A Yoshida
- College of Science and Engineering, Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo, Sagamihara, Kanagawa 252-5258, Japan
| | - K Yoshida
- Department of Electronic Information Systems, Shibaura Institute of Technology, 307 Fukasaku, Minuma, Saitama 337-8570, Japan
| |
Collapse
|
25
|
Korsmeier M, Donato F, Di Mauro M. Production cross sections of cosmic antiprotons in the light of new data from the NA61 and LHCb experiments. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.97.103019] [Citation(s) in RCA: 30] [Impact Index Per Article: 5.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
26
|
Korsmeier M, Donato F, Fornengo N. Prospects to verify a possible dark matter hint in cosmic antiprotons with antideuterons and antihelium. Int J Clin Exp Med 2018. [DOI: 10.1103/physrevd.97.103011] [Citation(s) in RCA: 31] [Impact Index Per Article: 5.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
27
|
|
28
|
Boschini MJ, Torre SD, Gervasi M, Grandi D, Jóhannesson G, Vacca GL, Masi N, Moskalenko IV, Pensotti S, Porter TA, Quadrani L, Rancoita PG, Rozza D, Tacconi M. HelMod in the Works: From Direct Observations to the Local Interstellar Spectrum of Cosmic-Ray Electrons. Astrophys J 2018; 854:94. [PMID: 34646044 PMCID: PMC8506982 DOI: 10.3847/1538-4357/aaa75e] [Citation(s) in RCA: 5] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/23/2023]
Abstract
The local interstellar spectrum (LIS) of cosmic-ray (CR) electrons for the energy range 1 MeV to 1 TeV is derived using the most recent experimental results combined with the state-of-the-art models for CR propagation in the Galaxy and in the heliosphere. Two propagation packages, GALPROP and HelMod, are combined to provide a single framework that is run to reproduce direct measurements of CR species at different modulation levels, and at both polarities of the solar magnetic field. An iterative maximum-likelihood method is developed that uses GALPROP-predicted LIS as input to HelMod, which provides the modulated spectra for specific time periods of the selected experiments for model-data comparison. The optimized HelMod parameters are then used to adjust GALPROP parameters to predict a refined LIS with the procedure repeated subject to a convergence criterion. The parameter optimization uses an extensive data set of proton spectra from 1997 to 2015. The proposed CR electron LIS accommodates both the low-energy interstellar spectra measured by Voyager 1 as well as the high-energy observations by PAMELA and AMS-02 that are made deep in the heliosphere; it also accounts for Ulysses counting rate features measured out of the ecliptic plane. The interstellar and heliospheric propagation parameters derived in this study agree well with our earlier results for CR protons, helium nuclei, and anti-protons propagation and LIS obtained in the same framework.
Collapse
Affiliation(s)
- M J Boschini
- INFN, Milano-Bicocca, Milano, Italy
- CINECA, Segrate, Milano, Italy
| | | | - M Gervasi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - D Grandi
- INFN, Milano-Bicocca, Milano, Italy
| | - G Jóhannesson
- Science Institute, University of Iceland, Dunhaga 3, IS-107 Reykjavik, Iceland
- NORDITA, Roslagstullsbacken 23, SE-106 91 Stockholm, Sweden
| | | | | | - I V Moskalenko
- Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - S Pensotti
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - T A Porter
- Hansen Experimental Physics Laboratory, Stanford University, Stanford, CA 94305, USA
- Kavli Institute for Particle Astrophysics and Cosmology, Stanford University, Stanford, CA 94305, USA
| | - L Quadrani
- INFN, Bologna, Italy
- Physics Department, University of Bologna, Bologna, Italy
| | | | - D Rozza
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| | - M Tacconi
- INFN, Milano-Bicocca, Milano, Italy
- Physics Department, University of Milano-Bicocca, Milano, Italy
| |
Collapse
|
29
|
Yalcin GC, Beck C. Generalized statistical mechanics of cosmic rays: Application to positron-electron spectral indices. Sci Rep 2018; 8:1764. [PMID: 29379055 PMCID: PMC5789131 DOI: 10.1038/s41598-018-20036-6] [Citation(s) in RCA: 31] [Impact Index Per Article: 5.2] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/28/2017] [Accepted: 01/12/2018] [Indexed: 11/13/2022] Open
Abstract
Cosmic ray energy spectra exhibit power law distributions over many orders of magnitude that are very well described by the predictions of q-generalized statistical mechanics, based on a q-generalized Hagedorn theory for transverse momentum spectra and hard QCD scattering processes. QCD at largest center of mass energies predicts the entropic index to be [Formula: see text]. Here we show that the escort duality of the nonextensive thermodynamic formalism predicts an energy split of effective temperature given by Δ [Formula: see text] MeV, where T H is the Hagedorn temperature. We carefully analyse the measured data of the AMS-02 collaboration and provide evidence that the predicted temperature split is indeed observed, leading to a different energy dependence of the e+ and e- spectral indices. We also observe a distinguished energy scale E* ≈ 50 GeV where the e+ and e- spectral indices differ the most. Linear combinations of the escort and non-escort q-generalized canonical distributions yield excellent agreement with the measured AMS-02 data in the entire energy range.
Collapse
Affiliation(s)
- G Cigdem Yalcin
- Department of Physics, Istanbul University, 34134, Vezneciler, Istanbul, Turkey
| | - Christian Beck
- School of Mathematical Sciences, Queen Mary University of London, Mile End Road, London, E1 4NS, UK.
| |
Collapse
|
30
|
DAMPE Collaboration. Direct detection of a break in the teraelectronvolt cosmic-ray spectrum of electrons and positrons. Nature 2017; 552:63-6. [PMID: 29186110 DOI: 10.1038/nature24475] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Abstract
High-energy cosmic-ray electrons and positrons (CREs), which lose energy quickly during their propagation, provide a probe of Galactic high-energy processes and may enable the observation of phenomena such as dark-matter particle annihilation or decay. The CRE spectrum has been measured directly up to approximately 2 teraelectronvolts in previous balloon- or space-borne experiments, and indirectly up to approximately 5 teraelectronvolts using ground-based Cherenkov γ-ray telescope arrays. Evidence for a spectral break in the teraelectronvolt energy range has been provided by indirect measurements, although the results were qualified by sizeable systematic uncertainties. Here we report a direct measurement of CREs in the energy range 25 gigaelectronvolts to 4.6 teraelectronvolts by the Dark Matter Particle Explorer (DAMPE) with unprecedentedly high energy resolution and low background. The largest part of the spectrum can be well fitted by a 'smoothly broken power-law' model rather than a single power-law model. The direct detection of a spectral break at about 0.9 teraelectronvolts confirms the evidence found by previous indirect measurements, clarifies the behaviour of the CRE spectrum at energies above 1 teraelectronvolt and sheds light on the physical origin of the sub-teraelectronvolt CREs.
Collapse
|
31
|
Direct detection of a break in the teraelectronvolt cosmic-ray spectrum of electrons and positrons. Nature 2017; 552:63-66. [DOI: 10.1038/nature24475] [Citation(s) in RCA: 287] [Impact Index Per Article: 41.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 06/28/2017] [Accepted: 10/04/2017] [Indexed: 11/09/2022]
|
32
|
Adriani O, Akaike Y, Asano K, Asaoka Y, Bagliesi MG, Bigongiari G, Binns WR, Bonechi S, Bongi M, Brogi P, Buckley JH, Cannady N, Castellini G, Checchia C, Cherry ML, Collazuol G, Di Felice V, Ebisawa K, Fuke H, Guzik TG, Hams T, Hareyama M, Hasebe N, Hibino K, Ichimura M, Ioka K, Ishizaki W, Israel MH, Javaid A, Kasahara K, Kataoka J, Kataoka R, Katayose Y, Kato C, Kawanaka N, Kawakubo Y, Krawczynski HS, Krizmanic JF, Kuramata S, Lomtadze T, Maestro P, Marrocchesi PS, Messineo AM, Mitchell JW, Miyake S, Mizutani K, Moiseev AA, Mori K, Mori M, Mori N, Motz HM, Munakata K, Murakami H, Nakahira S, Nishimura J, de Nolfo GA, Okuno S, Ormes JF, Ozawa S, Pacini L, Palma F, Papini P, Penacchioni AV, Rauch BF, Ricciarini SB, Sakai K, Sakamoto T, Sasaki M, Shimizu Y, Shiomi A, Sparvoli R, Spillantini P, Stolzi F, Takahashi I, Takayanagi M, Takita M, Tamura T, Tateyama N, Terasawa T, Tomida H, Torii S, Tsunesada Y, Uchihori Y, Ueno S, Vannuccini E, Wefel JP, Yamaoka K, Yanagita S, Yoshida A, Yoshida K, Yuda T. Energy Spectrum of Cosmic-Ray Electron and Positron from 10 GeV to 3 TeV Observed with the Calorimetric Electron Telescope on the International Space Station. Phys Rev Lett 2017; 119:181101. [PMID: 29219544 DOI: 10.1103/physrevlett.119.181101] [Citation(s) in RCA: 32] [Impact Index Per Article: 4.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/09/2017] [Indexed: 06/07/2023]
Abstract
First results of a cosmic-ray electron and positron spectrum from 10 GeV to 3 TeV is presented based upon observations with the CALET instrument on the International Space Station starting in October, 2015. Nearly a half million electron and positron events are included in the analysis. CALET is an all-calorimetric instrument with total vertical thickness of 30 X_{0} and a fine imaging capability designed to achieve a large proton rejection and excellent energy resolution well into the TeV energy region. The observed energy spectrum over 30 GeV can be fit with a single power law with a spectral index of -3.152±0.016 (stat+syst). Possible structure observed above 100 GeV requires further investigation with increased statistics and refined data analysis.
Collapse
Affiliation(s)
- O Adriani
- Department of Physics, University of Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - Y Akaike
- of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - K Asano
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - Y Asaoka
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
- JEM Utilization Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
| | - M G Bagliesi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - G Bigongiari
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - W R Binns
- Department of Physics, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - S Bonechi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - M Bongi
- Department of Physics, University of Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - P Brogi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - J H Buckley
- Department of Physics, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - N Cannady
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - G Castellini
- Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 50019 Sesto, Fiorentino, Italy
| | - C Checchia
- Department of Physics and Astronomy, University of Padova, Via Marzolo, 8, 35131 Padova, Italy
- INFN Sezione di Padova, Via Marzolo, 8, 35131 Padova, Italy
| | - M L Cherry
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - G Collazuol
- Department of Physics and Astronomy, University of Padova, Via Marzolo, 8, 35131 Padova, Italy
- INFN Sezione di Padova, Via Marzolo, 8, 35131 Padova, Italy
| | - V Di Felice
- University of Rome "Tor Vergata," Via della Ricerca Scientifica 1, 00133 Rome, Italy
- INFN Sezione di Rome "Tor Vergata," Via della Ricerca Scientifica 1, 00133 Rome, Italy
| | - K Ebisawa
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - H Fuke
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - T G Guzik
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - T Hams
- of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - M Hareyama
- St. Marianna University School of Medicine, 2-16-1, Sugao, Miyamae-ku, Kawasaki, Kanagawa 216-8511, Japan
| | - N Hasebe
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - K Hibino
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - M Ichimura
- Faculty of Science and Technology, Graduate School of Science and Technology, Hirosaki University, 3, Bunkyo, Hirosaki, Aomori 036-8561, Japan
| | - K Ioka
- Yukawa Institute for Theoretical Physics, Kyoto University, Kitashirakawa Oiwakecho, Sakyo, Kyoto 606-8502, Japan
| | - W Ishizaki
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - M H Israel
- Department of Physics, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - A Javaid
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - K Kasahara
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - J Kataoka
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - R Kataoka
- National Institute of Polar Research, 10-3, Midori-cho, Tachikawa, Tokyo 190-8518, Japan
| | - Y Katayose
- Faculty of Engineering, Division of Intelligent Systems Engineering, Yokohama National University, 79-5 Tokiwadai, Hodogaya, Yokohama 240-8501, Japan
| | - C Kato
- Faculty of Science, Shinshu University, 3-1-1 Asahi, Matsumoto, Nagano 390-8621, Japan
| | - N Kawanaka
- Hakubi Center, Kyoto University, Yoshida Honmachi, Sakyo-ku, Kyoto 606-8501, Japan
- Department of Astronomy, Graduate School of Science, Kyoto University, Kitashirakawa Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan
| | - Y Kawakubo
- College of Science and Engineering, Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo, Sagamihara, Kanagawa 252-5258, Japan
| | - H S Krawczynski
- Department of Physics, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - J F Krizmanic
- of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - S Kuramata
- Faculty of Science and Technology, Graduate School of Science and Technology, Hirosaki University, 3, Bunkyo, Hirosaki, Aomori 036-8561, Japan
| | - T Lomtadze
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
- University of Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - P Maestro
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - P S Marrocchesi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - A M Messineo
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
- University of Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - J W Mitchell
- Astroparticle Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - S Miyake
- Department of Electrical and Electronic Systems Engineering, National Institute of Technology, Ibaraki College, 866 Nakane, Hitachinaka, Ibaraki 312-8508, Japan
| | - K Mizutani
- Saitama University, Shimo-Okubo 255, Sakura, Saitama 338-8570, Japan
| | - A A Moiseev
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
- Department of Astronomy, University of Maryland, College Park, Maryland 20742, USA
| | - K Mori
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - M Mori
- Department of Physical Sciences, College of Science and Engineering, Ritsumeikan University, Shiga 525-8577, Japan
| | - N Mori
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - H M Motz
- International Center for Science and Engineering Programs, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - K Munakata
- Faculty of Science, Shinshu University, 3-1-1 Asahi, Matsumoto, Nagano 390-8621, Japan
| | - H Murakami
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - S Nakahira
- RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan
| | - J Nishimura
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - G A de Nolfo
- Heliospheric Physics Laboratory, NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - S Okuno
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - J F Ormes
- Department of Physics and Astronomy, University of Denver, Physics Building, Room 211, 2112 East Wesley Avenue, Denver, Colorado 80208-6900, USA
| | - S Ozawa
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - L Pacini
- Department of Physics, University of Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
- Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 50019 Sesto, Fiorentino, Italy
| | - F Palma
- University of Rome "Tor Vergata," Via della Ricerca Scientifica 1, 00133 Rome, Italy
- INFN Sezione di Rome "Tor Vergata," Via della Ricerca Scientifica 1, 00133 Rome, Italy
| | - P Papini
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - A V Penacchioni
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- ASI Science Data Center (ASDC), Via del Politecnico snc, 00133 Rome, Italy
| | - B F Rauch
- Department of Physics, Washington University, One Brookings Drive, St. Louis, Missouri 63130-4899, USA
| | - S B Ricciarini
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
- Institute of Applied Physics (IFAC), National Research Council (CNR), Via Madonna del Piano, 10, 50019 Sesto, Fiorentino, Italy
| | - K Sakai
- of Physics, University of Maryland, Baltimore County, 1000 Hilltop Circle, Baltimore, Maryland 21250, USA
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
| | - T Sakamoto
- College of Science and Engineering, Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo, Sagamihara, Kanagawa 252-5258, Japan
| | - M Sasaki
- CRESST and Astroparticle Physics Laboratory NASA/GSFC, Greenbelt, Maryland 20771, USA
- Department of Astronomy, University of Maryland, College Park, Maryland 20742, USA
| | - Y Shimizu
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - A Shiomi
- College of Industrial Technology, Nihon University, 1-2-1 Izumi, Narashino, Chiba 275-8575, Japan
| | - R Sparvoli
- University of Rome "Tor Vergata," Via della Ricerca Scientifica 1, 00133 Rome, Italy
- INFN Sezione di Rome "Tor Vergata," Via della Ricerca Scientifica 1, 00133 Rome, Italy
| | - P Spillantini
- Department of Physics, University of Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - F Stolzi
- Department of Physical Sciences, Earth and Environment, University of Siena, via Roma 56, 53100 Siena, Italy
- INFN Sezione di Pisa, Polo Fibonacci, Largo B. Pontecorvo, 3-56127 Pisa, Italy
| | - I Takahashi
- Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa 277-8583, Japan
| | - M Takayanagi
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - M Takita
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| | - T Tamura
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - N Tateyama
- Kanagawa University, 3-27-1 Rokkakubashi, Kanagawa, Yokohama, Kanagawa 221-8686, Japan
| | - T Terasawa
- RIKEN, 2-1 Hirosawa, Wako, Saitama 351-0198, Japan
| | - H Tomida
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - S Torii
- Research Institute for Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
- JEM Utilization Center, Human Spaceflight Technology Directorate, Japan Aerospace Exploration Agency, 2-1-1 Sengen, Tsukuba, Ibaraki 305-8505, Japan
- School of Advanced Science and Engineering, Waseda University, 3-4-1 Okubo, Shinjuku, Tokyo 169-8555, Japan
| | - Y Tsunesada
- Division of Mathematics and Physics, Graduate School of Science, Osaka City University, 3-3-138 Sugimoto, Sumiyoshi, Osaka 558-8585, Japan
| | - Y Uchihori
- National Institutes for Quantum and Radiation Science and Technology, 4-9-1 Anagawa, Inage, Chiba 263-8555, Japan
| | - S Ueno
- Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, 3-1-1 Yoshinodai, Chuo, Sagamihara, Kanagawa 252-5210, Japan
| | - E Vannuccini
- INFN Sezione di Florence, Via Sansone, 1-50019 Sesto, Fiorentino, Italy
| | - J P Wefel
- Department of Physics and Astronomy, Louisiana State University, 202 Nicholson Hall, Baton Rouge, Louisiana 70803, USA
| | - K Yamaoka
- Nagoya University, Furo, Chikusa, Nagoya 464-8601, Japan
| | - S Yanagita
- College of Science, Ibaraki University, 2-1-1 Bunkyo, Mito, Ibaraki 310-8512, Japan
| | - A Yoshida
- College of Science and Engineering, Department of Physics and Mathematics, Aoyama Gakuin University, 5-10-1 Fuchinobe, Chuo, Sagamihara, Kanagawa 252-5258, Japan
| | - K Yoshida
- Department of Electronic Information Systems, Shibaura Institute of Technology, 307 Fukasaku, Minuma, Saitama 337-8570, Japan
| | - T Yuda
- Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwa-no-Ha, Kashiwa, Chiba 277-8582, Japan
| |
Collapse
|
33
|
Donato F, Korsmeier M, Di Mauro M. Prescriptions on antiproton cross section data for precise theoretical antiproton flux predictions. Int J Clin Exp Med 2017. [DOI: 10.1103/physrevd.96.043007] [Citation(s) in RCA: 22] [Impact Index Per Article: 3.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/07/2022]
|
34
|
Jones LW. High energy physics and very high energy astrophysics. EPJ Web Conf 2017. [DOI: 10.1051/epjconf/201714505005] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
|
35
|
Spada FR. A new measurement of the Cosmic-Ray Electron Spectrum with Fermi-LAT. EPJ Web Conf 2017. [DOI: 10.1051/epjconf/201716401003] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
|
36
|
Duranti M. The AMS-02 detector on the International Space Station - The status after the first 5 years on orbit. EPJ Web Conf 2017. [DOI: 10.1051/epjconf/201713602004] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
|
37
|
Cummings AC, Stone EC, Heikkila BC, Lal N, Webber WR, Jóhannesson G, Moskalenko IV, Orlando E, Porter TA. GALACTIC COSMIC RAYS IN THE LOCAL INTERSTELLAR MEDIUM: VOYAGER 1 OBSERVATIONS AND MODEL RESULTS. Astrophys J 2016; 831:18. [PMID: 34646042 PMCID: PMC8507217 DOI: 10.3847/0004-637x/831/1/18] [Citation(s) in RCA: 60] [Impact Index Per Article: 7.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
Abstract
Since 2012 August Voyager 1 has been observing the local interstellar energy spectra of Galactic cosmic-ray nuclei down to 3 MeV nuc-1 and electrons down to 2.7 MeV. The H and He spectra have the same energy dependence between 3 and 346 MeV nuc-1, with a broad maximum in the 10-50 MeV nuc-1 range and a H/He ratio of 12.2 ± 0.9. The peak H intensity is ~15 times that observed at 1 AU, and the observed local interstellar gradient of 3-346 MeV H is -0.009 ± 0.055% AU-1, consistent with models having no local interstellar gradient. The energy spectrum of electrons (e - + e +) with 2.7-74 MeV is consistent with E -1.30±0.05 and exceeds the H intensity at energies below ~50 MeV. Propagation model fits to the observed spectra indicate that the energy density of cosmic-ray nuclei with >3 MeV nuc-1 and electrons with >3 MeV is 0.83-1.02 eV cm-3 and the ionization rate of atomic H is in the range of 1.51-1.64 × 10-17 s-1. This rate is a factor >10 lower than the ionization rate in diffuse interstellar clouds, suggesting significant spatial inhomogeneity in low-energy cosmic rays or the presence of a suprathermal tail on the energy spectrum at much lower energies. The propagation model fits also provide improved estimates of the elemental abundances in the source of Galactic cosmic rays.
Collapse
Affiliation(s)
- A C Cummings
- California Institute of Technology, Pasadena, CA 91125, USA
| | - E C Stone
- California Institute of Technology, Pasadena, CA 91125, USA
| | - B C Heikkila
- Goddard Space Flight Center. Greenbelt, MD 20771, USA
| | - N Lal
- Goddard Space Flight Center. Greenbelt, MD 20771, USA
| | - W R Webber
- New Mexico State University, Las Cruces, NM 88003, USA
| | | | - I V Moskalenko
- HEPL and KIPAC, Stanford University, Stanford, CA 94305, USA
| | - E Orlando
- HEPL and KIPAC, Stanford University, Stanford, CA 94305, USA
| | - T A Porter
- HEPL and KIPAC, Stanford University, Stanford, CA 94305, USA
| |
Collapse
|
38
|
Cowsik R, Madziwa-nussinov T. SPECTRAL INTENSITIES OF ANTIPROTONS AND THE NESTED LEAKY-BOX MODEL FOR COSMIC RAYS IN THE GALAXY. ACTA ACUST UNITED AC 2016; 827:119. [DOI: 10.3847/0004-637x/827/2/119] [Citation(s) in RCA: 31] [Impact Index Per Article: 3.9] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
|
39
|
|
40
|
|
41
|
Vecchi M. Recent results from the AMS-02 experiment. EPJ Web of Conferences 2015. [DOI: 10.1051/epjconf/201510501001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
|