Cosmic Rays and Their Radiative Processes in Numerical Cosmology
Abstract
A cosmological hydrodynamic code is described, which includes a routine to compute cosmic ray acceleration and transport in a simplified way. The routine was designed to follow explicitly diffusive acceleration at shocks, and second-order Fermi acceleration and adiabatic loss in smooth flows. Synchrotron cooling of the electron population can also be followed. The updated code is intended to be used to study the properties of nonthermal synchrotron emission and inverse Compton scattering from electron cosmic rays in clusters of galaxies, in addition to the properties of thermal bremsstrahlung emission from hot gas. The results of a test simulation using a grid of cells are presented, where cosmic rays and magnetic field have been treated passively and synchrotron cooling of cosmic ray electrons has not been included.
Cite
@article{arxiv.astro-ph/9912299,
title = {Cosmic Rays and Their Radiative Processes in Numerical Cosmology},
author = {Dongsu Ryu and Francesco Miniati and Tom W. Jones and Hyesung Kang},
journal= {arXiv preprint arXiv:astro-ph/9912299},
year = {2007}
}
Comments
3 pages, uses rmaa.cls, to appear in Proc. of the Conference on "Astrophysical Plasmas: Codes, Models and Observations", Eds. J. Franco, J. Arthur, N. Brickhouse, Rev.Mex.AA Conf. Series