固态天体物理学：X射线探测Interstellar Dust和气体性质
Solid State Astrophysics: Probing Interstellar Dust and Gas Properties with X-rays
摘要：
星际介质中气体和尘埃（固体和复杂分子）的丰度以及它们的组成和结构影响着几乎所有的天体物理学。从恒星形成到恒星风再到星系形成的基本过程都与金属的数量成比例。然而，在绝对和相对丰度以及这些丰度如何随环境变化方面仍然存在重大的不确定性，例如，恒星光球与星际介质（ISM）。虽然紫外线，光学，红外线和无线电研究已经大大提高了我们对ISM气体和尘埃的理解，但它们不能在所需的整个柱密度范围内提供统一的结果。相比之下，X射线将在宽范围的柱密度（log NH=20-24 cm^-2）下穿透冷（3 K）到热（100，000，000 K）宇宙中的气体和尘埃，留下反映组成气体的单个原子的光谱特征、分子或固体。* 因此，X射线是一种强大而可行的资源，可用于深入研究相对未开发的区域，以确定气体丰度和尘埃性质，例如通过吸收研究确定成分，电荷状态，结构和数量，以及通过散射晕确定分布。
英文摘要：
The abundances of gas and dust (solids and complex molecules) in the interstellar medium (ISM) as well as their composition and structures impact practically all of astrophysics. Fundamental processes from star formation to stellar winds to galaxy formation all scale with the number of metals. However, significant uncertainties remain in both absolute and relative abundances, as well as how these vary with environment, e.g., stellar photospheres versus the interstellar medium (ISM). While UV, optical, IR, and radio studies have considerably advanced our understanding of ISM gas and dust, they cannot provide uniform results over the entire range of column densities needed. In contrast, X-rays will penetrate gas and dust in the cold (3K) to hot (100,000,000K) Universe over a wide range of column densities (log NH=20-24 cm^-2), imprinting spectral signatures that reflect the individual atoms which make up the gas, molecule or solid. *X-rays therefore are a powerful and viable resource for delving into a relatively unexplored regime for determining gas abundances and dust properties such as composition, charge state, structure, and quantity via absorption studies, and distribution via scattering halos.*
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