Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1991
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.249..439k&link_type=abstract
Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 249, April 1, 1991, p. 439-451. University of Minnesota
Astronomy and Astrophysics
Astronomy
61
Charged Particles, Energetic Particles, Galactic Cosmic Rays, Particle Acceleration, Supernova Remnants, Energy Transfer, Particle Diffusion, Shock Wave Attenuation, Signal To Noise Ratios
Scientific paper
The time-dependent acceleration of cosmic ray particles by the Fermi, first-order diffusive shock process in supernova remnants is examined. The convection-diffusion transport equation for the cosmic ray particles has been numerically solved self-consistently with the gas dynamic equations for the underlying flow. A model SNR characterized by an explosion energy of 10 to the 51st ergs, an ejected mass of 10 solar masses and an ISM gas density of 0.003/cu cm is followed through the adiabatic, Sedov-Taylor phase. A wide range of diffusion coefficients is considered. From these numerical results, it is concluded that the observed spectrum of galactic cosmic rays (a power law with q of about 4.2 - 4.3 extending up to 10 to the 14th eV) may be explained by diffusive acceleration in SNR if the diffusion coefficient is as small as the Bohm limit. At the same time, the cosmic rays can absorb about 30 percent of the explosion energy. That is apparently enough to replenish the galactic cosmic rays. Although the dynamical feedback of the cosmic ray pressure modifies the shock structure to some degree, the shock is still dominated by the gas pressure at late times, so the temperature of the postshock gas should be large enough to agree with X-ray observations of SNRs.
Jones Thomas W.
Kang Hyesung
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