Thermal X-ray emission and cosmic-ray production in young supernova remnants

被引:107
作者
Decourchelle, A [1 ]
Ellison, DC
Ballet, J
机构
[1] Ctr Etud Saclay, Serv Astrophys Orme Merisiers, F-91191 Gif Sur Yvette, France
[2] N Carolina State Univ, Dept Phys, Raleigh, NC 27695 USA
关键词
acceleration of particles; hydrodynamics; ISM : abundances; ISM : individual (Kepler's Supernova); supernova remnants; X-rays : ISM;
D O I
10.1086/318167
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We have developed a simple model to investigate the modifications of the hydrodynamics and nonequilibrium ionization X-ray emission in young supernova remnants due to nonlinear particle acceleration. In nonlinear, diffusive shock acceleration, the heating of the gas to X-ray-emitting temperatures is strongly coupled to the acceleration of cosmic-ray ions. If the acceleration is efficient and a significant fraction of the shock ram energy ends up in cosmic rays, compression ratios will be higher and the shocked temperature lower than test particle, Rankine-Hugoniot relations predict. We illustrate how particle acceleration impacts the interpretation of X-ray data using the X-ray spectra of Kepler's remnant, observed by ASCA and the Rossi X-Ray Timing Explorer. The thermal X-ray emission provides important constraints on the efficiency of particle acceleration, in complement to nonthermal emission. X-ray data from Chandra and XMM-Newton, plus radio observations, will be essential to quantify nonlinear effects.
引用
收藏
页码:L57 / L60
页数:4
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