论文标题
超新星残留物的电子加速度
Electron acceleration at supernova remnants
论文作者
论文摘要
据信超新星残留物（SNR）会产生大多数银河宇宙射线（CRS）。 SNRS具有通过扩散冲击加速度（DSA）加速CRS的非相关性无碰撞冲击，其中颗粒通过与冲击阵线的重复相互作用通过反复相互作用而获得了能量。由于DSA理论涉及预先存在的轻度能量颗粒，因此需要一种先前的加速方式，尤其是对于电子而言。电子注入仍然是最麻烦，尚未解决的问题之一，我们对它的物理理解对于完全理解SNR的物理学至关重要。为了研究负责预系的任何电子尺度现象，我们需要一种能够解决这些小动力学尺度和粒子中的模拟（PIC）模拟的方法。在这里，我报告了利用非权利主义高马赫数冲击的动力学模拟取得的最新成就。我讨论了SNR冲击的物理学如何取决于冲击参数（例如，冲击倾斜，马赫数，离子与电子质量比）以及负责电子加热和加速的过程。
Supernova remnants (SNRs) are believed to produce the majority of galactic cosmic rays (CRs). SNRs harbor non-relativistic collisionless shocks responsible for acceleration of CRs via diffusive shock acceleration (DSA), in which particles gain their energies via repeated interactions with the shock front. As the DSA theory involves pre-existing mildly energetic particles, a means of pre-acceleration is required, especially for electrons. Electron injection remains one of the most troublesome and still unresolved issues and our physical understanding of it is essential to fully comprehend the physics of SNRs. To study any electron-scale phenomena responsible for pre-acceleration, we require a method capable of resolving these small kinetic scales and Particle-in-cell (PIC) simulations fulfill this criterion. Here I report on the latest achievements made by utilising kinetic simulations of non-relativistic high Mach number shocks. I discuss how the physics of SNR shocks depend on the shock parameters (e.g., the shock obliquity, Mach numbers, the ion-to-electron mass ratio) as well as processes responsible for the electron heating and acceleration.
