Cosmic-Ray Protons Accelerated at Cosmological Shocks and Their Impact on Groups and Clusters of Galaxies
The Astrophysical Journal American Astronomical Society 559:1 (2001) 59-69
Winds and shocks in galaxy clusters: Shock acceleration on an intergalactic scale
AIP Conference Proceedings 558:1 (2001) 436-447
Cosmic rays and their radiative processes in numerical cosmology
Revista Mexicana de Astronomia y Astrofisica: Serie de Conferencias 9 (2000) 305-307
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 ows. 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 1283 cells are presented, where cosmic rays and magnetic field have been treated passively and synchrotron cooling of cosmic ray electrons has not been included.Three-dimensional Magnetohydrodynamic Numerical Simulations of Cloud-Wind Interactions
The Astrophysical Journal American Astronomical Society 543:2 (2000) 775-786
Properties of Cosmic Shock Waves in Large‐Scale Structure Formation
The Astrophysical Journal American Astronomical Society 542:2 (2000) 608-621