模拟X射线双星的加速和辐射过程
Simulating acceleration and radiation processes in X-ray binaries
摘要：
微类星体的高能辐射被认为是来自高能粒子。根据光谱状态，这些粒子的分布可以是具有高温（通常为100 keV）的热的，或者是非热的，并且延伸到甚至更高的能量。高能等离子体的性质是由一个丰富的微观物理涉及粒子粒子碰撞和粒子光子相互作用。我们提出了一个新的代码开发，以解决相对论等离子体的演化。这个单区代码侧重于微观物理学，并解决粒子和光子的耦合动力学方程，包括康普顿散射，同步辐射发射和吸收，对生产和湮灭，韧致辐射发射和吸收，库仑相互作用，以及额外的粒子加速和加热的处方。它可以特别描述机制，如同步自吸收和库仑碰撞的热化。利用该程序，我们研究了不同的加速过程，即热加热，非热加速和随机加速，是否可以再现微类星体的不同光谱状态。给出了初步结果。
英文摘要：
The high energy emission of microquasars is thought to originate from high energy particles. Depending on the spectral state, the distribution of these particles can be thermal with a high temperature (typically 100 keV) or non-thermal and extending to even higher energy. The properties of high energy plasmas are governed by a rich microphysics involving particle-particle collisions and particles-photons interactions. We present a new code developed to address the evolution of relativistic plasmas. This one-zone code focuses on the microphysics and solves the coupled kinetic equations for particles and photons, including Compton scattering, synchrotron emission and absorption, pair production and annihilation, bremsstrahlung emission and absorption, Coulomb interactions, and prescriptions for additional particle acceleration and heating. It can in particular describe mechanisms such a thermalisation by synchrotron self-absorption and Coulomb collisions. Using the code, we investigate whether various acceleration processes, namely thermal heating, non-thermal acceleration and stochastic acceleration, can reproduce the different spectral states of microquasars. Premilinary results are presented.
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