Electron Heating in Perpendicular Low-beta Shocks
Electron Heating in Perpendicular Low-beta Shocks
复制标题
垂直低贝塔冲击中的电子加热
作者：
A. Tran;L. Sironi
无碰撞冲击太阳风、星际冲击波和热气体渗透星系团中的热电子。有多少冲击加热传递给电子而不是离子，以及什么等离子体物理控制电子加热？我们使用全动力学粒子细胞代码模拟二维垂直冲击。对于磁声马赫数和等离子体β，激波后电子/离子温度比随着 的增加从1减小到0.1。在代表性的 激波中，电子分两步加热到绝热压缩之上：离子尺度将电子加速成沿 的流，然后通过类似双流的不稳定性松弛。平行加热主要是由波引起的； -垂直加热主要是准静态场的绝热压缩。
Collisionless shocks heat electrons in the solar wind, interstellar blast waves, and hot gas permeating galaxy clusters. How much shock heating goes to electrons instead of ions, and what plasma physics controls electron heating? We simulate 2D perpendicular shocks with a fully kinetic particle-in-cell code. For magnetosonic Mach number and plasma beta , the post-shock electron/ion temperature ratio decreases from 1 to 0.1 with increasing . In a representative , shock, electrons heat above adiabatic compression in two steps: ion-scale accelerates electrons into streams along , which then relax via two-stream-like instability. The -parallel heating is mostly induced by waves; -perpendicular heating is mostly adiabatic compression by quasi-static fields.
DOI：
10.3847/1538-4357/ab03d7
发表时间：
2019-01
期刊：
The Astrophysical Journal
影响因子：
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作者：
M. Rowan;L. Sironi;R. Narayan
通讯作者：
M. Rowan;L. Sironi;R. Narayan