高能粒子激波加速与超新星遗迹辐射分布形态

宇宙中高能粒子的加速过程与宇宙线起源属于天体物理领域内的热门课题。超新星遗迹作为银河系宇宙线粒子起源的主要候选体，尽管观测已遍及全波段，但其中发生的非相对论激波加速粒子机制、高能伽玛射线起源及各种辐射分布形态产生原因等关键问题尚不明确。. 本项目拟通过hybrid particle-in-cell (PIC)数值模拟方法从第一性原理出发，研究非相对论激波中的粒子加速过程；同时，对超新星遗迹在不同环境下的演化过程开展三维MHD数值模拟研究。结合hybrid PIC数值模拟结果及辐射机制理论，对超新星遗迹的动力学演化和辐射分布形态开展研究，解释观测到的动力学特征及各种超新星遗迹辐射分布形态产生原因，掌握超新星遗迹周围星际介质特征，探究前身星及伴星的星风对遗迹辐射分布形态的影响。

The acceleration processes of charged particles in the universe and the origin of cosmic rays belong to the hot topics in astrophysics. Although the observations on supernova remnants(SNRs), which are the primary candidates of the origin of the Galactic cosmic rays, extend to all wavebands, some key points, such as the acceleration of particles at the nonrelativistic shocks, the origin of the gamma-rays from the SNRs and the mechanisms to produce the various SNRs' morphologies of emission are still unclear now.. This project intends to investigate the particle acceleration at the nonrelativisic shocks from first principles throught the hybrid PIC simulation; moreover, the evolution of the SNRs in different environments are studied via 3D MHD simunation. Combined with the results from the hybrid PIC simulations and the theory of the radiative mechanisms, the dynamical properties of the SNRs and the morphologies of emission can be obtained, and both the detected dynamical properties and the various morphologies can be explained. Furthermore, the properties of the insterstellare medium around the SNRs, and the impact of the winds either from the progenitors or from the companion stars can be derived.