Cosmic rays in supernova remnants. I - Transport coefficients

Details Cosmic rays in supernova remnants. I - Transport coefficients Cosmic rays in supernova remnants. I - Transport coefficients

Sep 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...232..473m&link_type=abstract

Astrophysical Journal, Part 1, vol. 232, Sept. 1, 1979, p. 473-484.

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11

Cosmic Rays, Nebulae, Supernova Remnants, Transport Properties, Particle Acceleration, Particle Interactions, Stellar Models, Topology, Wave Interaction

Scientific paper

The problem of cosmic-ray transport in supernova remnants (SNRs) is discussed under the assumption that wave-particle interaction is parasitic, i.e., the waves produced by the cosmic-ray streaming can be neglected. Calculations of the maximum 'active age' of SNRs (i.e., the time during which the initially excited wave activity dies down) show that appreciable post-acceleration of cosmic rays may be possible, which in turn may lead to a replenishment of low-energy cosmic rays that otherwise are lost through ionization of the interstellar medium. Transport coefficients in coordinate and energy space are calculated in a realistic SNR model using the most plausible assumptions about wave activity and wave-particle interaction. This allows a quantitative determination of energy losses and gains to be made as a function of cosmic-ray rigidity.

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