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 ##IMG## [http://ej.iop.org/images/2041-8205/900/2/L36/apjlabb19cieqn1.gif] {${{ \mathcal M }}_{\mathrm{ms}}\sim 1\mbox{--}10$} and plasma beta ##IMG## [http://ej.iop.org/images/2041-8205/900/2/L36/apjlabb19cieqn2.gif] {${\beta }_{{\rm{p}}}\lesssim 4$} , the post-shock electron/ion temperature ratio ##IMG## [http://ej.iop.org/images/2041-8205/900/2/L36/apjlabb19cieqn3.gif] {${T}_{{\rm{e}}}/{T}_{{\rm{i}}}$} decreases from 1 to 0.1 with increasing ##IMG## [http://ej.iop.org/images/2041-8205/900/2/L36/apjlabb19cieqn4.gif] {${{ \mathcal M }}_{\mathrm{ms}}$} . In a re...

中文翻译：

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垂直低β冲击中的电子加热

无碰撞冲击会在太阳风，星际爆炸波和热气渗透星系团中加热电子。多少冲击加热会传递给电子而不是离子，并且什么等离子体物理学会控制电子加热？我们使用完全动态的单元格内粒子代码模拟2D垂直冲击。对于磁声马赫数## IMG ## [http://ej.iop.org/images/2041-8205/900/2/L36/apjlabb19cieqn1.gif] {$ {{\ mathcal M}} _ {\ mathrm { ms}} \ sim 1 \ mbox {-} 10 $}和血浆beta ## IMG ## [http://ej.iop.org/images/2041-8205/900/2/L36/apjlabb19cieqn2.gif] {$ {\ beta} _ {{\ rm {p}}} \ lesssim 4 $}，震后电子/离子温度比## IMG ## [http://ej.iop.org/images/2041 -8205 / 900/2 / L36 / apjlabb19cieqn3.gif] {$ {T} _ {{\ rm {e}}} / {T} _ {{\ rm {i}}} $}从1减少到0.1 ## IMG ## [http://ej.iop.org/images/2041-8205/900/2/L36/apjlabb19cieqn4。gif] {$ {{\ mathcal M}} _ {\ mathrm {ms}} $}。在...