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《中国物理C》（英文）编辑部
2024年10月30日
Chinese Physics C> 2016, Vol. 40> Issue(11) : 115001 DOI: 10.1088/1674-1137/40/11/115001

On the contribution of a hard galactic plane component to the excesses of secondary particles

  • 1.

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

  • The standard model of cosmic ray propagation has been very successful in explaining all kinds of galactic cosmic ray spectra. However, high precision measurement have recently revealed an appreciable discrepancy between data and model expectations, from spectrum observations of gamma-rays, e+/e- and probably the B=C ratio starting from ~10 GeV energy . In this work, we propose that a hard galactic plane component, supplied by the fresh cosmic ray sources and detained by local magnetic elds, can contribute additional secondary particles interacting with local materials. By properly choosing the intensity and spectral index of the harder component up to multi-T eV energy , a two-component gamma-ray spectrum is obtained and agrees very well with the observation. Simultaneously , the expected neutrino numbers from the galactic plane could contribute ~60% of IceCube observed neutrino number below a few hundreds of TeV under our model. In addition to these studies, we nd that the same pp-collision process responsible for the excess gamma ray emission could account for a signi cant amount of the positron excess, but a more detailed mechanism is needed for a full agreement. It is expected that the excesses in the p=p and B=C ratio will show up when energy is above ~10 GeV. We look forward this model being tested in the near future by new observations from AMS02, IceCube, AS-gamma, HA WC and future  experiments such as LHASSO, HiSCORE and CTA.
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Yi-Qing Guo, Hong-Bo Hu and Zhen Tian. On the contribution of a hard galactic plane component to the excesses of secondary particles[J]. Chinese Physics C, 2016, 40(11): 115001. doi: 10.1088/1674-1137/40/11/115001
Yi-Qing Guo, Hong-Bo Hu and Zhen Tian. On the contribution of a hard galactic plane component to the excesses of secondary particles[J]. Chinese Physics C, 2016, 40(11): 115001.  doi: 10.1088/1674-1137/40/11/115001 shu
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Received: 2015-09-17
Revised: 2016-07-28
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    Natural Sciences Foundation of China (11135010)

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On the contribution of a hard galactic plane component to the excesses of secondary particles

  • 1. Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing 100049, China
  • Received Date: 2015-09-17
  • Accepted Date: 2016-07-28
  • Available Online: 2016-11-05
Fund Project:  Natural Sciences Foundation of China (11135010)

Abstract: The standard model of cosmic ray propagation has been very successful in explaining all kinds of galactic cosmic ray spectra. However, high precision measurement have recently revealed an appreciable discrepancy between data and model expectations, from spectrum observations of gamma-rays, e+/e- and probably the B=C ratio starting from ~10 GeV energy . In this work, we propose that a hard galactic plane component, supplied by the fresh cosmic ray sources and detained by local magnetic elds, can contribute additional secondary particles interacting with local materials. By properly choosing the intensity and spectral index of the harder component up to multi-T eV energy , a two-component gamma-ray spectrum is obtained and agrees very well with the observation. Simultaneously , the expected neutrino numbers from the galactic plane could contribute ~60% of IceCube observed neutrino number below a few hundreds of TeV under our model. In addition to these studies, we nd that the same pp-collision process responsible for the excess gamma ray emission could account for a signi cant amount of the positron excess, but a more detailed mechanism is needed for a full agreement. It is expected that the excesses in the p=p and B=C ratio will show up when energy is above ~10 GeV. We look forward this model being tested in the near future by new observations from AMS02, IceCube, AS-gamma, HA WC and future  experiments such as LHASSO, HiSCORE and CTA.

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