Astronomy and Astrophysics – Astronomy
Scientific paper
Nov 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...251..597d&link_type=abstract
Astronomy and Astrophysics (ISSN 0004-6361), vol. 251, no. 2, Nov. 1991, p. 597-610.
Astronomy and Astrophysics
Astronomy
40
Cosmic Rays, Gamma Ray Astronomy, Radiant Cooling, Stellar Evolution, Supernova Remnants, Particle Acceleration, Radiation Pressure, Shock Fronts, Stellar Envelopes
Scientific paper
This paper numerically follows the evolution of SNRs taking the nonlinear effects of particle acceleration in shock waves into account. Several SNR models with different efficiencies for the conversion of the SN explosion energy E(SN) into cosmic rays (CRs) are discussed. The gamma-ray fluxes from pi(0) decay yield 10 exp -10 ph/sq cm/s for a typical SNR with a small amount of CR energy at a time of 300 yrs and increase almost as R(s)-cubed due to geometric effects. SNRs with higher fractions of CRs or SNRs evolving into a medium of higher ambient density produce gamma-ray fluxes of up to about 10 exp -6 ph/sq cm/s. The radius of the forward shock varies between 1 pc and 70 pc for these gamma-ray fluxes. In the latter case the gamma-ray fluxes are almost constant between 10,000 and 10 exp 6 yrs. The effects of radiative cooling alter the overall energetics of an SNR, but between 10 and 30 percent of the E(SN) is converted into high-energy particles.
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