Particle acceleration by ultra-relativistic shocks: theory and simulations

Details Particle acceleration by ultra-relativistic shocks: theory and simulations Particle acceleration by ultra-relativistic shocks: theory and simulations

2001-07-27

arxiv.org/abs/astro-ph/0107530v1

Mon.Not.Roy.Astron.Soc. 328 (2001) 393

Astronomy and Astrophysics

Astrophysics

Accepted by MNRAS, 39 pages, 10 figures, uses latex macro mn.sty

Scientific paper

10.1046/j.1365-8711.2001.04851.x

We consider the acceleration of charged particles near ultra-relativistic shocks, with Lorentz factor Gamma_s >> 1. We present simulations of the acceleration process and compare these with results from semi-analytical calculations. We show that the spectrum that results from acceleration near ultra-relativistic shocks is a power law, N(E) \propto E^{-s}, with a nearly universal value s \approx 2.2 - 2.3 for the slope of this power law. We confirm that the ultra-relativistic equivalent of Fermi acceleration at a shock differs from its non-relativistic counterpart by the occurence of large anisotropies in the distribution of the accelerated particles near the shock. In the rest frame of the upstream fluid, particles can only outrun the shock when their direction of motion lies within a small loss cone of opening angle theta_c \approx 1/Gamma_s around the shock normal. We also show that all physically plausible deflection or scattering mechanisms can change the upstream flight direction of relativistic particles originating from downstream by only a small amount: Delta theta ~ 1/Gamma_s. This limits the energy change per shock crossing cycle to Delta E ~ E, except for the first cycle where particles originate upstream. In that case the upstream energy is boosted by a factor ~ Gamma_s^2 for those particles that are scattered back across the shock into the upstream region.

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