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《中国物理C》（英文）编辑部
2024年10月30日
Chinese Physics C> 2018, Vol. 42> Issue(7) : 075001 DOI: 10.1088/1674-1137/42/7/075001

Cosmic ray electron spectrum due to the dispersion ofinjection spectrum

  • 1.

     School of Physics and Technology, Wuhan University, Wuhan 430072, China

  • 2.

     Physics Department of the Science School, Tibet University, Lhasa 850000, China

  • 3.

     Key Laboratory of Cosmic Rays(Tibet University), Ministry of Education, Lhasa 850000, China

  • 4.

      Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China

  • 5.

     Physics Department of the Science School, Tibet University, Lhasa 850000, China

  • 6.

     Key Laboratory of Cosmic Rays(Tibet University), Ministry of Education, Lhasa 850000, China

  • 7.

      School of Physics and Technology, Wuhan University, Wuhan 430072, China

  • The cosmic-ray total electron spectrum (electrons plus positrons) has been measured precisely up to TeV energies, with more interesting features found. Exhaustive analyses of the electron spectrum strongly support a spectral hardening above 100 GeV, rather than a featureless single power-law, which is confirmed by the most recent observations. Meanwhile, the measurements of the DAMPE satellite have verified the presence of a knee-like structure around 1 TeV in the electron spectrum, resembling the cosmic-ray knee. In this paper, we establish a physical model in which the observed electron spectrum is composed of a superposition of CR sources with various spectral indices and high-energy cutoffs. The dispersion of the power index is assumed to be Gaussian, while the cutoff energy Ec follows a power-law distribution. These simple ideas can account naturally for both the hundred-GeV excess and the TeV spectral break.
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  • References

    [1] M. A. DuVernois, S. W. Barwick, J. J. Beatty et al, ApJ, 559: 296303 (2001)
    [2] J. J. Beatty, A. Bhattacharyya, C. Bower et al, Physical Review Letters, 93(24): 241102 (2004)
    [3] M. Aguilar, J. Alcaraz et al (AMS-01 Collaboration), Physics Letters B, 646: 145154 (2007)
    [4] J. Chang, J. H. Adams, H. S. Ahn et al, Nature, 456: 362365 (2008)
    [5] S. Torii, T. Yamagami, T. Tamura et al, High-energy electron observations by PPB-BETS flight in Antarctica. ArXiv e-prints, September 2008
    [6] O. Adriani, G. C. Barbarino, G. A. Bazilevskaya et al, Nature, 458: 607609 (2009)
    [7] A. A. Abdo, M. Ackermann, M. Ajello et al, Physical Review Letters, 102(18): 181101 (2009)
    [8] L. Accardo, M. Aguilar, D. Aisa et al, Physical Review Letters, 113(12): 121101 (2014)
    [9] M. Aguilar, D. Aisa, A. Alvino et al, Physical Review Letters, 113(12): 121102 (2014)
    [10] X.-J. Bi, P.-F. Yin, and Q. Yuan, Frontiers of Physics, 8: 794-827 (2013)
    [11] I. Cholis and D. Hooper, Phys. Rev. D, 88(2): 023013 (2013)
    [12] Q. Yuan and X.-J. Bi, Physics Letters B, 727: 17 (2013)
    [13] L. Feng, R.-Z. Yang, H.-N. He et al, Physics Letters B, 728: 250255 (2014)
    [14] X. Li, Z.-Q. Shen, B.-Q. Lu et al, Physics Letters B, 749: 267-271 (2015)
    [15] A. D. Panov, J. H. Adams, H. S. Ahn et al, Bulletin of the Russian Academy of Sciences, Physics, 73: 564567 (2009)
    [16] O. Adriani, G. C. Barbarino, G. A. Bazilevskaya et al, Science, 332: 69 (2011)
    [17] H. S. Ahn, P. Allison, M. G. Bagliesi et al, ApJl, 714: L89L93 (2010)
    [18] Y. S. Yoon, H. S. Ahn, P. S. Allison et al, ApJ, 728: 122 (2011)
    [19] M. Aguilar, D. Aisa, B. Alpat et al, Physical Review Letters, 114(17): 171103 (2015)
    [20] M. Aguilar, D. Aisa, B. Alpat et al, Physical Review Letters, 115(21): 211101 (2015)
    [21] M. Aguilar, L. Ali Cavasonza, G. Ambrosi et al, Phys. Rev. Lett., 120: 021101 (2018)
    [22] S. Abdollahi, M. Ackermann, M. Ajello et al, Phys. Rev. D, 95(8): 082007 (2017)
    [23] DAMPE Collaboration, G. Ambrosi, Q. An et al, Nature, 552: 6366 (2017)
    [24] W. Liu, X.-J. Bi, S.-J. Lin, B.-B. Wang, and P.-F. Yin, Phys. Rev. D, 96(2): 023006 (2017)
    [25] V. Ptuskin, V. Zirakashvili, and E.-S. Seo, ApJ, 763: 47 (2013)
    [26] F. Aharonian, A. G. Akhperjanian, U. Barres de Almeida et al, Physical Review Letters, 101(26): 261104 (2008)
    [27] F. Aharonian, A. G. Akhperjanian, G. Anton et al, AA, 508: 561564 (2009)
    [28] D. Borla Tridon, International Cosmic Ray Conference, 6: 47 (2011)
    [29] D. Staszak (VERITAS Collaboration), In 34th International Cosmic Ray Conference (ICRC2015), volume 34 of International Cosmic Ray Conference, page 411, July 2015
    [30] M. Amenomori, X. J. Bi, D. Chen et al, ApJ, 678: 11651179 (2008)
    [31] M. G. Aartsen, R. Abbasi, Y. Abdou et al, Phys. Rev. D, 88(4):042004 (2013)
    [32] G. Vannoni, S. Gabici, and F. A. Aharonian, AA, 497: 1726 (2009)
    [33] S. Thoudam and J. R. Hrandel, MNRAS, 414: 14321438 (2011)
    [34] Y. Ohira, R. Yamazaki, N. Kawanaka, and K. Ioka, MNRAS, 427: 91102 (2012)
    [35] K. Fang, X.-J. Bi, and P.-F. Yin, ApJ, 854: 57 (2018)
    [36] R. Schlickeiser and J. Ruppel, New Journal of Physics, 12(3):033044 (2010)
    [37] L . Stawarz, V. Petrosian, and R. D. Blandford, ApJ, 710: 236-247 (2010)
    [38] N. Kawanaka, K. Ioka, and M. M. Nojiri. Is Cosmic Ray Electron Excess from Pulsars Spiky or Smooth?: Continuous and Multiple Electron/Positron Injections. ApJ, 710:958963, February 2010.
    [39] K. Fang, B.-B. Wang, X.-J. Bi, S.-J. Lin, and P.-F. Yin, ApJ, 836: 172 (2017)
    [40] B.-B. Wang, X.-J. Bi, S.-J. Lin, and P.-f. Yin, Explanations of the DAMPE high energy electron/positron spectrum in the dark matter annihilation and pulsar scenarios, ArXiv e-prints, July 2017
    [41] Q. Yuan, L. Feng, P.-F. Yin et al, Interpretations of the DAMPE electron data, ArXiv e-prints, November 2017
    [42] K. Fang, X.-J. Bi, P.-F. Yin, and Q. Yuan, Two-zone diffusion of electrons and positrons from Geminga explains the positron anomaly, ArXiv e-prints, March 2018
    [43] C. Jin, W. Liu, H.-B. Hu, and Y.-Q. Guo, On the PeV knee of cosmic rays spectrum and TeV cutoff of electron spectrum, ArXiv e-prints, November 2016
    [44] S. P. Reynolds, ARAA, 46: 89126 (2008)
    [45] G. Dubner and E. Giacani, AA Rev., 23: 3 (2015)
    [46] P. Slane, A. Bykov, D. C. Ellison, G. Dubner, and D. Castro, Space Sci. Rev., 188: 187210 (2015)
    [47] A. M. Bykov, D. C. Ellison, A. Marcowith, and S. M. Osipov, Space Sci. Rev., 214: 41 (2018)
    [48] D. A. Green, Bulletin of the Astronomical Society of India, 42: 4758 (2014)
    [49] M. Pohl and J. A. Esposito, ApJ, 507: 327338 (1998)
    [50] I. Bsching, M. Pohl, and R. Schlickeiser, AA, 377: 1056-1062 (2001)
    [51] Q. Yuan, B. Zhang, and X.-J. Bi, Phys. Rev. D, 84(4): 043002 (2011)
    [52] M. A. Malkov, P. H. Diamond, and R. Z. Sagdeev, Nature Communications, 2: 194 (2011)
    [53] D. Maurin, R. Taillet, F. Donato et al, Galactic Cosmic Ray Nuclei as a Tool for Astroparticle Physics, ArXiv Astrophysics e-prints, December 2002
    [54] A. W. Strong, I. V. Moskalenko, and V. S. Ptuskin, Annual Review of Nuclear and Particle Science, 57: 285327 (2007)
    [55] L. J. Gleeson and W. I. Axford, ApJ, 154: 1011 (1968)
    [56] M. Aguilar, D. Aisa, B. Alpat et al, Physical Review Letters, 113(22): 221102 (2014)
    [57] E. G. Berezhko and G. F. Krymskii, Soviet Physics Uspekhi, 31: 2751 (1988)
    [58] P. A. Becker, T. Le, and C. D. Dermer, ApJ, 647: 539551 (2006)
    [59] V. N. Zirakashvili and F. Aharonian, AA, 465: 695702 (2007)
    [60] P. Blasi, MNRAS, 402: 28072816 (2010)
    [61] T. Kobayashi, Y. Komori, K. Yoshida, and J. Nishimura, ApJ, 601: 340351 (2004)
    [62] A. U. Abeysekara, A. Albert, R. Alfaro et al, Science, 358: 911914 (2017)

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Tian-Lu Chen, Wei Liu, Qi Gao, Mao-Yuan Liu, Hai-Jin Li, Danzengluobu and Ying Shi. Cosmic ray electron spectrum due to the dispersion ofinjection spectrum[J]. Chinese Physics C, 2018, 42(7): 075001. doi: 10.1088/1674-1137/42/7/075001
Tian-Lu Chen, Wei Liu, Qi Gao, Mao-Yuan Liu, Hai-Jin Li, Danzengluobu and Ying Shi. Cosmic ray electron spectrum due to the dispersion ofinjection spectrum[J]. Chinese Physics C, 2018, 42(7): 075001.  doi: 10.1088/1674-1137/42/7/075001 shu
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Received: 2018-03-22
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    Supported by National Natural Sciences Foundation of China (11663006, 11747316, 11135010, 11405182) and the Research Project of Chinese Ministry of Education (213036A)

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Cosmic ray electron spectrum due to the dispersion ofinjection spectrum

  • 1. School of Physics and Technology, Wuhan University, Wuhan 430072, China
  • 2. Physics Department of the Science School, Tibet University, Lhasa 850000, China
  • 3. Key Laboratory of Cosmic Rays(Tibet University), Ministry of Education, Lhasa 850000, China
  • 4.  Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
  • 5. Physics Department of the Science School, Tibet University, Lhasa 850000, China
  • 6. Key Laboratory of Cosmic Rays(Tibet University), Ministry of Education, Lhasa 850000, China
  • 7.  School of Physics and Technology, Wuhan University, Wuhan 430072, China
  • Received Date: 2018-03-22
  • Available Online: 2018-07-05
Fund Project:  Supported by National Natural Sciences Foundation of China (11663006, 11747316, 11135010, 11405182) and the Research Project of Chinese Ministry of Education (213036A)

Abstract: The cosmic-ray total electron spectrum (electrons plus positrons) has been measured precisely up to TeV energies, with more interesting features found. Exhaustive analyses of the electron spectrum strongly support a spectral hardening above 100 GeV, rather than a featureless single power-law, which is confirmed by the most recent observations. Meanwhile, the measurements of the DAMPE satellite have verified the presence of a knee-like structure around 1 TeV in the electron spectrum, resembling the cosmic-ray knee. In this paper, we establish a physical model in which the observed electron spectrum is composed of a superposition of CR sources with various spectral indices and high-energy cutoffs. The dispersion of the power index is assumed to be Gaussian, while the cutoff energy Ec follows a power-law distribution. These simple ideas can account naturally for both the hundred-GeV excess and the TeV spectral break.

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