Statistics – Computation
Scientific paper
Nov 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...363..499j&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 363, Nov. 10, 1990, p. 499-514. Research supported by the University of Min
Statistics
Computation
63
Computational Astrophysics, Cosmic Rays, Shock Waves, Two Fluid Models, Astronomical Models, Evolution (Development), Particle Acceleration, Time Dependence
Scientific paper
Extensive numerical simulations of cosmic-ray-mediated shocks have been carried out in the two-fluid model, examining the time-dependent evolution of the shocks in plane-parallel and spherical symmetric geometries. The plane shocks eventually reach equilibrium states in a time controlled by the development of the shock precursor. The time is typically two orders of magnitude greater than the cosmic-ray diffusion time, and depends on the degree of shock restructuring required to attain equilibrium. Spherical shocks are not found to reach equilibrium. It is found that supernova shocks can transfer about 10 percent of their blast energy through diffusive processes into cosmic rays at the end of the adiabatic Sedov-Taylor phase.
Jones Thomas W.
Kang Hyesung
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