arXiv 2104.002642021-04-01astro-ph.EPastro-ph.SR

EXOPLINES：棕矮星和巨系外行星大气的分子吸收截面数据库

EXOPLINES: Molecular Absorption Cross-Section Database for Brown Dwarf and Giant Exoplanet Atmospheres

Ehsan Gharib-Nezhad, Aishwarya R. Iyer, Michael R. Line, Richard S. Freedman, Mark S. Marley, Natasha E. Batalha

备注：: accepted in ApJS. 44 pages, 17 figures, 7 tables. Comments are welcome
DOI：: 10.3847/1538-4365/abf504

摘要：

恒星、亚恒星和行星大气模型都对输入不透明度高度敏感。各种最先进的恒星/行星模型之间的世代差异主要是因为不完整和过时的原子/分子线列表。在这里，我们提出了一个数据库的预先计算的吸收截面的所有同位素的关键大气分子相关的晚型恒星，棕矮星，和行星大气：MgH，AlH，CaH，TiH，CrH，FeH，SiO，TiO，VO和H2O。计算的不透明度的压力和温度范围在10 $^{-6}$-3000巴和75- 4000 K之间，在可能的情况下，它们的光谱范围在0.25-$μ$ m之间。对于没有压力加宽数据的情况，我们使用碰撞理论来弥合差距。我们还探讨了在超热木星和M-矮星大气的背景下，从不同的线列表计算的吸收截面的影响。使用1-D自洽的辐射-对流热化学平衡模型，我们报告显着的变化，在理论光谱和温度分布的亚恒星大气。与2000 K代表性的超热木星，我们报告的变化高达320和80 ppm的透射和热发射光谱，分别。对于一个3000 K的M-矮星，我们发现的差异高达125 $\%$的光谱。我们发现，最显着的差异出现由于TiO线列表的选择，主要低于1 $μ$ m。总之，我们提出了（1）一个预先计算的分子吸收截面数据库，（2）量化由于线列表差异而在表征亚恒星/系外行星大气时出现的偏差，因此突出了正确和完整的不透明度对于最终应用于高精度光谱学和光度学的重要性。

英文摘要：

Stellar, substellar, and planetary atmosphere models are all highly sensitive to the input opacities. Generational differences between various state-of-the-art stellar/planetary models are primarily because of incomplete and outdated atomic/molecular line-lists. Here we present a database of pre-computed absorption cross-sections for all isotopologues of key atmospheric molecules relevant to late-type stellar, brown dwarf, and planetary atmospheres: MgH, AlH, CaH, TiH, CrH, FeH, SiO, TiO, VO, and H2O. The pressure and temperature ranges of the computed opacities are between 10$^{-6}$--3000~bar and 75--4000~K, and their spectral ranges are 0.25--330~$μ$m for many cases where possible. For cases with no pressure-broadening data, we use collision theory to bridge the gap. We also probe the effect of absorption cross-sections calculated from different line lists in the context of Ultra-Hot Jupiter and M-dwarf atmospheres. Using 1-D self-consistent radiative-convective thermochemical equilibrium models, we report significant variations in the theoretical spectra and thermal profiles of substellar atmospheres. With a 2000 K representative Ultra-Hot Jupiter, we report variations of up to 320 and 80 ppm in transmission and thermal emission spectra, respectively. For a 3000 K M-dwarf, we find differences of up to 125$\%$ in the spectra. We find that the most significant differences arise due to the choice of TiO line-lists, primarily below 1$μ$m. In sum, we present (1) a database of pre-computed molecular absorption cross-sections, and (2) quantify biases that arise when characterizing substellar/exoplanet atmospheres due to line list differences, therefore highlighting the importance of correct and complete opacities for eventual applications to high precision spectroscopy and photometry.

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