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Introduction

  • Hidetoshi Sano
Chapter
Part of the Springer Theses book series (Springer Theses)

Abstract

Cosmic rays are charged and highly energetic particles mainly comprising protons, with \(\sim \)10\(\%\) helium and 1 \(\%\) electrons and ionized nuclei. Understanding the origin and acceleration mechanism of cosmic rays has been one of the most important challenges in astrophysics over the past century because cosmic rays have a significant influence on the interstellar space via ionizing / heating the interstellar gas. Supernova remnants are the most likely candidates for acceleration of Galactic cosmic rays (\(E\,<\,10^{15.5}\) eV, the so called “knee”), however, the sources of cosmic ray protons have still not been firmly identified observationally. In this Chapter, I introduce recent theoretical and observational knowledge of cosmic ray acceleration in the supernova remnants.

Keywords

Spectral Index Shock Front Supernova Remnant Inverse Compton Scattering Diffusive Shock Acceleration 
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 2017

Authors and Affiliations

  1. 1.Department of PhysicsNagoya UniversityNagoyaJapan

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