We have developed a cosmic-ray (CR) shock code in one dimensional spherical geometry in which the particle distribution and the gas flow can be followed numerically in a frame comoving with a spherical shock. We find the spatial grid spacing required for numerical convergence is less stringent in this code, compared to the typical Eulerian code. This is because the shock stays in the same grid zone in the comoving frame. In addition, the adaptive mesh refinement and the coarse-grained momentum volume method have been implement into the new code in order to achieve the highest possible computational efficiency. Using this code with the realistic Bohm type diffusion model we have calculated the CR acceleration and the nonlinear feedback at supernova remnant shocks during Sedov-Taylor stage. Similarly to plane-parallel shocks with M8 ̃ 10-15, about 50% of the kinetic energy that has passed through the shock is converted to CR energy.
|Original language||English (US)|
|Number of pages||4|
|State||Published - 2005|
|Event||29th International Cosmic Ray Conference, ICRC 2005 - Pune, India|
Duration: Aug 3 2005 → Aug 10 2005
|Other||29th International Cosmic Ray Conference, ICRC 2005|
|Period||8/3/05 → 8/10/05|
Bibliographical noteFunding Information:
HK was supported by the Korea Research Foundation Grant funded by Korea Government (MOEHRD, Basic Research Promotion Fund) (R04-2004-000-100590) and by KOSEF through the Astrophysical Research Center for the Structure and Evolution of Cosmos (ARCSEC). TWJ is supported at the University of Minnesota by NASA grant NNG05GF57G and by the Minnesota Supercomputing Institute.