论文标题
恒星和行星的风和磁层：相似性和差异
Winds and magnetospheres of stars and planets: similarities and differences
论文作者
论文摘要
恒星和行星都可以通过膨胀的空白流失量失去质量，这通常由形成周围磁层的磁场限制或引导。理解，巨大恒星的强风是由恒星辐射动量的线散射驱动的，而在阳光下，甚至在较低的质量恒星中，质量较弱的质量损失源于机械加热的电晕的热膨胀。在这样的低质量恒星周围的系外行星中，辐射加热和风相互作用会导致其大气的热膨胀或机械消融。恒星磁层是由风流的内部捕获而产生的，而行星磁层通常是由恒星风的外部冲击来影响的。但是在这两种情况下，压力都可以驱动磁重新连接，从而导致可观察到的特征，例如X射线耀斑和无线电爆发。这篇评论的目的是概述这些过程的基本物理，重点是它们的相似性和对星球与行星的区别。
Both stars and planets can lose mass through an expansive wind outflow, often constrained or channeled by magnetic fields that form a surrounding magnetosphere. The very strong winds of massive stars are understood to be driven by line-scattering of the star's radiative momentum, while in the Sun and even lower-mass stars a much weaker mass loss arises from the thermal expansion of a mechanically heated corona. In exoplanets around such low-mass stars, the radiative heating and wind interaction can lead to thermal expansion or mechanical ablation of their atmospheres. Stellar magnetospheres result from the internal trapping of the wind outflow, while planetary magnetospheres are typically shaped by the external impact from the star's wind. But in both cases the stressing can drive magnetic reconnection that results in observable signatures such as X-ray flares and radio outbursts. This review will aim to give an overview of the underlying physics of these processes with emphasis on their similarities and distinctions for stars vs. planets.
