Very-High-Energy Solar Gamma Rays From Cosmic-Ray Interactions

ORAL

Abstract

Cosmic-ray induced gamma rays from the Sun has been observed up to ~100 GeV. However, there are no theoretical predictions beyond 10 GeV. We provide the first calculation of the hadronic disk component in TeV-PeV, where solar magnetic fields can be ignored. We also consider the leptonic gamma-ray halo, taking into account electrons from local pulsars. With Fermi and soon HAWC & LHAASO observations, our results provide new insights on local cosmic rays, solar magnetic fields, and solar dark matter studies.

*BZ is supported by OSU Fowler Fellowship. KN and FB are supported by NSF Grant PHY-1404311. AK is supported by NSF GRFP Grant No. DGE-1321846. CR is supported by the Korea Neutrino Research Center. KN is also supported by the OSU Presidential Fellowship.

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Authors

  • Bei Zhou

    • Center of Cosmology and AstroParticle Physics (CCAPP), Ohio State University (OSU), Columbus, Ohio 43210, USA

  • Kenny Ng

    • Center of Cosmology and AstroParticle Physics (CCAPP), Ohio State University (OSU), Columbus, Ohio 43210, USA

  • John Beacom

    • Center of Cosmology and AstroParticle Physics (CCAPP), Ohio State University (OSU), Columbus, Ohio 43210, USA

  • Annika Peter

    • Center of Cosmology and AstroParticle Physics (CCAPP), Ohio State University (OSU), Columbus, Ohio 43210, USA

  • Cartsen Rott

    • Department of Physics, Sungkyunkwan University, Suwon 440-746, Korea