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Monte Carlo shock-like solutions to the Boltzmann equation with collective scattering
Ellison, D. C.; Eichler, D.
AA(NASA, Goddard Space Flight Center, Greenbelt; Maryland, University, College Park, MD), AB(Negev, University, Beersheba, Israel; Maryland, University, College Park, MD)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 286, Nov. 15, 1984, p. 691-701. (ApJ Homepage)
Publication Date:
NASA/STI Keywords:
Cosmic Rays, Elastic Scattering, Interplanetary Space, Monte Carlo Method, Particle Acceleration, Shock Waves, Mach Number, Mean Free Path, Partial Pressure, Plasma-Particle Interactions, Relativistic Particles
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The results of Monte Carlo simulations of steady state shocks generated by a collision operator that isotropizes the particles by means of elastic scattering in some locally defined frame of reference are presented. The simulations include both the back reaction of accelerated particles on the inflowing plasma and the free escape of high-energy particles from finite shocks. Energetic particles are found to be naturally extracted out of the background plasma by the shock process with an efficiency in good quantitative agreement with an earlier analytic approximation (Eichler, 1983 and 1984) and observations (Gosling et al., 1981) of the entire particle spectrum at a quasi-parallel interplanetary shock. The analytic approximation, which allows a self-consistent determination of the effective adiabatic index of the shocked gas, is used to calculate the overall acceleration efficiency and particle spectrum for cases where ultrarelativistic energies are obtained. It is found that shocks of the strength necessary to produce galactic cosmic rays put approximately 15 percent of the shock energy into relativistic particles.

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