Atomic and Molecular Opacities for Brown Dwarf and Giant Planet Atmospheres
Atomic and Molecular Opacities for Brown Dwarf and Giant Planet Atmospheres
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DOI：
10.1086/508708
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发表时间：
2006-07
期刊：
影响因子：
--
通讯作者：
C. Sharp;A. Burrows
中科院分区：
文献类型：
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作者：
C. Sharp;A. Burrows
我们提出了一个全面的理论和实践的不透明度计算，从红外到紫外线需要生成棕矮星和系外巨行星的大气模型。提出了使用现有谱线列表和不同格式的光谱数据库的方法，并提供了在代表性温度/压力点上最重要的分子和原子的吸收不透明度与波长的关系图。推导、讨论和分析了电子、旋转振动、无束缚、无束缚、自由-自由和碰撞诱导的跃迁和单色不透明。研究对象包括碱金属、铁、重金属氧化物、金属氢化物、H2、H2O、CH4、CO、NH3、H2S、PH3和具有代表性的颗粒。一旦得到了所有成分的单色吸收截面，就必须先得到化学丰度，然后才能对所得产物进行求和以得到总不透明度。因此，我们包括热化学，技术和数据库需要得出平衡丰度和提供一些样本结果的回顾。
We present a comprehensive description of the theory and practice of opacity calculations from the infrared to the ultraviolet needed to generate models of the atmospheres of brown dwarfs and extrasolar giant planets. Methods for using existing line lists and spectroscopic databases in disparate formats are presented, and plots of the resulting absorptive opacities versus wavelength for the most important molecules and atoms at representative temperature/pressure points are provided. Electronic, rovibrational, bound-free, bound-bound, free-free, and collision-induced transitions and monochromatic opacities are derived, discussed, and analyzed. The species addressed include the alkali metals, iron, heavy metal oxides, metal hydrides, H2, H2O, CH4, CO, NH3, H2S, PH3, and representative grains. Once monochromatic absorption cross sections for all constituents have been derived, chemical abundances have to be obtained before the resulting product can be summed to obtain total opacities. Hence, we include a review of the thermochemistry, techniques, and databases needed to derive equilibrium abundances and provide some sample results.