恒星的X射线光谱学
X-Ray Spectroscopy of Stars
摘要：
基本上所有光谱类别的非简并恒星都是软X射线源。位于主序星较冷部分的低质量恒星和它们在主序星之前的前身，通过数量来定义星系中占主导地位的恒星星族。它们的X射线光谱在最广泛的意义上让人联想到来自日冕的X射线光谱。从冷恒星发出的X射线确实是由类似于太阳日冕等离子体的被磁性捕获的热气体发出的。日冕的结构，它的热分层和几何范围可以解释基于各种光谱诊断。在前主序星中已经发现了新的特征，其中一些可能与恒星表面的吸积冲击、由于X射线照射而在拱星盘上产生的荧光或恒星外流中的冲击加热有关。大质量、炽热的恒星显然主导着与银河系星际介质的相互作用：它们是电离辐射、机械能和星系化学富集的主要来源。高能辐射允许探测这些恒星中某些最重要的工作过程，并限制它们最奇特的功能：星风。在这里，我们回顾了最近的进展，我们的理解，通过X射线光谱的研究，特别是高分辨率的光谱，现在可以从XMM-牛顿和钱德拉。我们解决的问题有关的日冕结构，耀斑，日冕等离子体的组成，X射线生产的吸积流和外流，X射线从单一的OB型恒星，大规模的双星，磁热物体和演变的WR星。
英文摘要：
(abridged) Non-degenerate stars of essentially all spectral classes are soft X-ray sources. Low-mass stars on the cooler part of the main sequence and their pre-main sequence predecessors define the dominant stellar population in the galaxy by number. Their X-ray spectra are reminiscent, in the broadest sense, of X-ray spectra from the solar corona. X-ray emission from cool stars is indeed ascribed to magnetically trapped hot gas analogous to the solar coronal plasma. Coronal structure, its thermal stratification and geometric extent can be interpreted based on various spectral diagnostics. New features have been identified in pre-main sequence stars; some of these may be related to accretion shocks on the stellar surface, fluorescence on circumstellar disks due to X-ray irradiation, or shock heating in stellar outflows. Massive, hot stars clearly dominate the interaction with the galactic interstellar medium: they are the main sources of ionizing radiation, mechanical energy and chemical enrichment in galaxies. High-energy emission permits to probe some of the most important processes at work in these stars, and put constraints on their most peculiar feature: the stellar wind. Here, we review recent advances in our understanding of cool and hot stars through the study of X-ray spectra, in particular high-resolution spectra now available from XMM-Newton and Chandra. We address issues related to coronal structure, flares, the composition of coronal plasma, X-ray production in accretion streams and outflows, X-rays from single OB-type stars, massive binaries, magnetic hot objects and evolved WR stars.
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