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《中国物理C》 2016-01
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Spatial dependent diffusion of cosmic rays and the excess of primary electrons derived from high precision measurements by AMS-02

Chao Jin;Yi-Qing Guo;Hong-Bo Hu;School of Physical Engineering, Zhengzhou University;Key Laboratory of Particle Astrophysics, Institute of High Energy Physics,Chinese Academy of Sciences;  
The precise spectra of Cosmic Ray(CR) electrons and positrons have been published by the measurement of AMS-02. It is reasonable to regard the difference between the electron and positron spectra(?Φ = Φ_(e-)-Φ_(e+)) as being dominated by primary electrons. The resulting electron spectrum shows no sign of spectral softening above 20 GeV, which is in contrast with the prediction of the standard model of CR propagation. In this work, we generalize the analytic one-dimensional two-halo model of diffusion to a three-dimensional realistic calculation by implementing spatial variant diffusion coefficients in the DRAGON package. As a result, we can reproduce the spectral hardening of protons observed by several experiments, and predict an excess of high energy primary electrons which agrees with the measurement reasonably well. Unlike the break spectrum obtained for protons, the model calculation predicts a smooth electron excess and thus slightly over-predicts the flux from tens of GeV to 100 GeV. To understand this issue, further experimental and theoretical studies are necessary.
【Fund】: Supported by Natural Sciences Foundation of China(11135010)
【CateGory Index】: O572.322
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142284,Protvino,Russia;LPNHE,IN2P3-CNRS et Universites de Paris 6 et 7,F-75252 Paris,France;Max-Planck-Institute of Physics,80805 Munich,Germany;Department of Physics,University of Washington,Seattle,WA 98195,USA;Ludwig-Maximilians-Universitat,Fakultdt für Physik,Schellingstr.4,D-80799 München,Germany;Enrico Fermi Institute and Department of Physics,University of Chicago,Chicago,IL 60637-1433,USA;Department of Physics,Syracuse University,Syracuse,NY,13244,USA;Department of Physics,Columbia University,538 W.120th Street,New York,NY,10027 USA;High Energy Physics Group,Blackett Laboratory,Imperial College,Prince Consort Road,London SW7 2AZ,UK;Jefferson Lab,12000 Jefferson Ave.,Newport News,VA 23606,USA;Department of Physics,University of Virginia,PO Box 400714,Charlottesville,VA 22904,USA;Fermi National Accelerator Laboratory,P.O.Box 500,Batavia,IL 60510,USA;Kavli Institute for Cosmological Physics,University of Chicago,Chicago,IL 60637-1433,USA;Department of Physics and 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Diego,La Jolla,CA 92093,USA;INFN Sezione di Cagliari,Cittadella Universitaria di Monserrato,1-09042 Monserrato(CA),Italy;Department of Physics and Astronomy,Louisana State University,Baton Rouge,LA 70803;Fysikum,Stockholms Universitet,AlbaNova University Centre,SE-106 91 Stockholm,Sweden;INAF-OATS,via G.B.Tiepolo 11,34143 Trieste,Italy;DESY,D-15735 Zeuthen,Germany;The Space Sciences Laboratory(SSL),University of California,7 Gauss Way,Berkeley,CA 94720,USA;Department of Physics,University of California,Berkeley,CA 94720,USA;Brown University,Department of Physics,182 Hope Street,Providence,RI 02912,USA;INFN,Sez.di Milano-Bicocca,Piazza delta Scienza,3,1-20126 Milano,Italy;Dpto.de Fisica Teorica y del Cosmos & C.A.F.P.E.,Universidad de Granada,18071 Granada,Spain;PRISMA Cluster of Excellence and Mainz Institute for Theoretical Physics,Johannes Gutenberg University,D-55099 Mainz,Germany;Department of Particle Physics and Astrophysics,Weizmann Institute of Science,Rehovot 761000 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Laboratory,J.J.Thomson Avenue,Cambridge CB3 OHE,UK;Department of Astronomy and CCAPP,The Ohio State University,140 W.18th Ave.,Columbus,OH 43210,USA;Dept.of Physics,Colorado School of Mines,Golden Colorado,80401 USA;Department of Physics,Carnegie Mellon University,Pittsburgh,PA 15213,USA;STFC Rutherford Appleton Laboratory,Didcot,OX11 OQX,UK;Department of Physics,George Washington University Virginia Campus,Ashburn,VA 20147-2604,USA;IHEP,Chinese Academy of Sciences;California Institute of Technology,High Energy Physics,MC 256-48,Pasadena,CA 91125,USA;;COSMIC RAYS[J];中国物理C;2014-09
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