Radiative cooling rates, ion fractions, molecule abundances, and line emissivities including self-shielding and both local and metagalactic radiation fields
Radiative cooling rates, ion fractions, molecule abundances, and line emissivities including self-shielding and both local and metagalactic radiation fields
复制标题
辐射冷却速率、离子分数、分子丰度和线发射率，包括自屏蔽以及局部和超星系辐射场
DOI：
10.1093/mnras/staa2172
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发表时间：
2020
影响因子：
4.8
通讯作者：
J. Schaye
中科院分区：
文献类型：
--
作者：
S. Ploeckinger;J. Schaye
我们使用光谱合成代码cloudy来将气体在红移（z = 0-9）、温度（log T[K] = 1-9.5）、金属丰度（log Z/Z = −4 -+0.5，Z = 0）和密度（$\log n_{\mathrm{H}}[\，\mathrm{cm}^{-3}] = -8$ − +6）的广泛范围内的性质制成表格。因此，这包括具有星际、环星系和星系间介质特性的气体。气体暴露在红移相关的UV/X射线背景下，而对于自屏蔽的低温气体（即ISM气体），添加了星际辐射场和宇宙射线。辐射场被密度和温度相关的气体和尘埃柱衰减。受观测到的星星形成规律的激励，这种气柱密度也决定了星际辐射场的强度和宇宙线密度。的电离平衡，分子分数，冷却速率，线发射率，和平衡温度计算自洽。我们包括尘埃，宇宙射线，星际辐射场逐步研究它们的相对影响。这些公开可用的表格是流体动力学模拟的理想选择。它们可以单独使用，也可以耦合到非平衡网络中的一个子集。该版本包括一个C例程来读取和插入表，以及一个易于使用的python图形用户界面来浏览表。
We use the spectral synthesis code cloudy to tabulate the properties of gas for an extensive range in redshift (z = 0–9), temperature (log T[K] = 1–9.5), metallicity (log Z/Z⊙ = −4 – +0.5, Z = 0), and density ($\log n_{\mathrm{H}}[\, \mathrm{cm}^{-3}] = -8$ − +6). This therefore includes gas with properties characteristic of the interstellar, circumgalactic, and intergalactic media. The gas is exposed to a redshift-dependent UV/X-ray background, while for the self-shielded lower-temperature gas (i.e. ISM gas), an interstellar radiation field and cosmic rays are added. The radiation field is attenuated by a density- and temperature-dependent column of gas and dust. Motivated by the observed star formation law, this gas column density also determines the intensity of the interstellar radiation field and the cosmic ray density. The ionization balance, molecule fractions, cooling rates, line emissivities, and equilibrium temperatures are calculated self-consistently. We include dust, cosmic rays, and the interstellar radiation field step-by-step to study their relative impact. These publicly available tables are ideal for hydrodynamical simulations. They can be used stand alone or coupled to a non-equilibrium network for a subset of elements. The release includes a C routine to read in and interpolate the tables, as well as an easy-to-use python graphical user interface to explore the tables.
影响因子：
4.8
作者：
Xuejian Shen;P. Hopkins;C. Faucher-Giguère;D. Alexander;G. Richards;N. Ross;R. Hickox
通讯作者：
Xuejian Shen;P. Hopkins;C. Faucher-Giguère;D. Alexander;G. Richards;N. Ross;R. Hickox
影响因子：
4.8
作者：
Faucher-Giguere, Claude-Andre
通讯作者：
Faucher-Giguere, Claude-Andre
影响因子：
4.9
作者：
Bisbas, Thomas G.;van Dishoeck, Ewine F.;Zhang, Zhi-Yu
通讯作者：
Zhang, Zhi-Yu