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Detection of VHE γ-Rays and Neutrinos

  • Tadashi Kifune
  • Masaki Mori

Abstract

Observation of Galactic γ-rays was first proposed by Hayakawa and Morrison at the end of 1950’s. Cosmic rays collide with interstellar matter producing γ-rays and, thereby, the observation can give an estimate of the amount of interstellar matter together with the existence of high energy protons. Unfortunately, the expected γ-ray flux is small when estimated from the known cosmic ray intensity. However, a more intense and more detectable flux of γ-rays might be expected if a considerable amount of antiprotons exist in the Galaxy as suggested by Morrison. At that time, radio wave detection had just started to uncover high energy phenomena in the universe. One mechanism of radio wave emission is synchrotron radiation, and in this case it was concluded that high energy electrons as well as magnetic fields exist in various objects at far distances from us. In addition to the high energy processes due to electrons, observation of γ-rays reveals high energy phenomena including high energy protons at far places in the universe.

Keywords

Active Galactic Nucleus Atmospheric Neutrino Galactic Disc Neutrino Flux Crab Nebula 
These keywords were added by machine and not by the authors. This process is experimental and the keywords may be updated as the learning algorithm improves.

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Copyright information

© Springer Japan 1994

Authors and Affiliations

  • Tadashi Kifune
    • 1
  • Masaki Mori
    • 2
  1. 1.ICRRUniversity of TokyoJapan
  2. 2.Department of PhysicsMiyagi University of EducationJapan

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