非辐射激波中的非麦克斯韦质子速度分布
Non-Maxwellian Proton Velocity Distributions in Nonradiative Shocks
摘要：
非辐射超新星遗迹激波的巴耳末线剖面提供了测量激波后质子速度分布的手段。虽然大多数分析假设麦克斯韦速度分布，这是不可能正确的。特别是，穿过激波并在下游被电离的中性原子形成了一种类似于太阳风中拾取离子的非热分布。我们预测的H α线配置文件的组合拾取质子和普通的冲击质子，我们认为在何种程度上，这种分布可能会影响来自H α配置文件的冲击参数。麦克斯韦假设可能导致对激波速度的低估，最高可达15%。拾取离子布居的各向同性产生波能量，并且我们发现，对于最有利的参数，这种能量可以显着加热热粒子。足够精确的配置文件可以约束的强度和方向的磁场在冲击等离子体，我们讨论了从高斯分布的扭曲预期在第谷的超新星遗迹。
英文摘要：
The Balmer line profiles of nonradiative supernova remnant shocks provide the means to measure the post-shock proton velocity distribution. While most analyses assume a Maxwellian velocity distribution, this is unlikely to be correct. In particular, neutral atoms that pass through the shock and become ionized downstream form a nonthermal distribution similar to that of pickup ions in the solar wind. We predict the H alpha line profiles from the combination of pickup protons and the ordinary shocked protons, and we consider the extent to which this distribution could affect the shock parameters derived from H alpha profiles. The Maxwellian assumption could lead to an underestimate of shock speed by up to about 15%. The isotropization of the pickup ion population generates wave energy, and we find that for the most favorable parameters this energy could significantly heat the thermal particles. Sufficiently accurate profiles could constrain the strength and direction of the magnetic field in the shocked plasma, and we discuss the distortions from a Gaussian profile to be expected in Tycho's supernova remnant.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
