Shock-Generated Cosmic Rays in AMR Hydro/N-body Cosmological Simulations

Details Shock-Generated Cosmic Rays in AMR Hydro/N-body Cosmological Simulations Shock-Generated Cosmic Rays in AMR Hydro/N-body Cosmological Simulations

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.9618s&link_type=abstract

American Astronomical Society, AAS Meeting #211, #96.18; Bulletin of the American Astronomical Society, Vol. 39, p.903

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Shock waves in cosmological simulations arise due to supersonic accretion onto large scale structures such as filaments and galaxy clusters as well as from complex flows within the clusters themselves. Along with thermal dissipation due to shock heating, cosmic rays can be generated through diffusive shock acceleration (DSA). By using the results from one-dimensional DSA simulations, we compute the energy dissipation into non-thermal cosmic ray particles from shocks. This cosmic ray pressure is found to be a significant fraction of the total thermal pressure, suggesting that in order to perform precision cosmological studies with galaxy clusters, this additional non-thermal physics must be included.
Here we present new numerical simulations using a Hydro/N-body Adaptive Mesh Refinement (AMR) code, ENZO, to analyze cosmic ray generation. Whereas previous analyses have been performed on a fixed grid or within individual galaxy clusters, we are able for the first time to study cosmic ray generation over a spatial dynamic range of up to 2^8. In addition, a shock-finding algorithm has been developed that does not rely on studying shock waves in each of the three coordinate directions separately. Instead, our algorithm casts a ray in the direction of the shock propagation and then determines the Mach number using Rankine-Hyugenot jump conditions for the adiabatic gas.

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