Abstract
Supernova remnants, owing to their strong shock waves, are likely sources of Galactic cosmic rays. Studies of supernova remnants in X-rays and gamma rays provide us with new insights into the acceleration of particles to high energies. This paper reviews the basic physics of supernova remnant shocks and associated particle acceleration and radiation processes. In addition, the study of supernova remnant populations in nearby galaxies and the implications for Galactic cosmic ray distribution are discussed.
Highlights
Supernova remnants (SNR) are among the most beautiful astronomical objects, presenting various kinds of morphologies
Most of the SNRs in our Galaxy were discovered as non-thermal, extended radio sources with a flux spectrum described by a power-law Sν ∝ να with α ≈ −0.5
Sites of particle accelerations in the interstellar space are the strong shock waves in SNRs, which are the remains of supernova explosions and heat the ambient interstellar medium (ISM) and distribute heavy elements that were processed inside the progenitor star throughout the Galaxy
Summary
Supernova remnants (SNR) are among the most beautiful astronomical objects, presenting various kinds of morphologies. Most of the SNRs in our Galaxy were discovered as non-thermal, extended radio sources with a flux spectrum described by a power-law Sν ∝ να with α ≈ −0.5. This emission was explained as synchrotron radiation emitted by a non-thermal, power-law population of relativistic electrons with N (E) = KE−s electrons cm−3 erg−1. These electrons produce a power-law photon distribution with α = (1 − s)/2, s = 2 for α = −0.5
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