自洽 MSG（MARCS-StaticWeather-GGchem）冷恒星、亚恒星及系外行星模型大气网格
A grid of self-consistent MSG (MARCS-StaticWeather-GGchem) cool stellar, sub-stellar, and exoplanetary model atmospheres
AI总结：
本文构建了 300K 至 3000K 冷恒星、亚恒星及系外行星的自洽一维模型大气网格 MSG，通过迭代耦合 MARCS、StaticWeather 和 GGchem 三个代码，纳入云形成、化学非平衡和恒星辐照，揭示了比传统 M、L、T 序列更复杂的光谱分类特征。
摘要：
本文计算了一套自洽的一维模型大气网格，覆盖冷恒星、亚恒星天体及系外行星，有效温度范围为 300K 至 3000K，包含云形成、化学非平衡效应以及恒星辐照。这些模型被称为 MSG，因为它们基于三个经过充分检验的代码之间的迭代耦合：MARCS 恒星大气代码、StaticWeather 云形成代码和 GGchem 化学平衡代码。该网格包含最新的分子和原子不透明度、云形成和先进的化学平衡计算，并在低温下采用了新的数值方法以确保稳健收敛。MARCS 辐射转移与 GGchem 化学平衡计算之间的耦合，使得较温暖的模型能够有效地基于电子压达到收敛，而较冷的模型则基于气压达到收敛，从而能够在非常宽的有效温度范围内对恒星、亚恒星和系外行星天体进行自洽建模。本文描述了模型的基本细节，并给出了有云模型、受辐照模型以及基于非平衡化学的模型的示例。模型中 TiO、H2O、CH4、NH3 及其他分子的相对丰度的定性变化遵循观测上定义的 M、L、T（和 Y）序列，但揭示了更复杂且随深度变化的丰度变化，因此光谱分类依赖于更多参数。与 StaticWeather 云计算的自洽耦合，使得能够对成核过程与观测到的不同光谱波段相对变暗进行详细比较，并为潜在系外行星生物特征的新识别方法提供了高级应用。
英文摘要：
Computation of a grid of self consistent 1D model atmospheres of cool stars, sub-stellar objects and exoplanets in the effective temperature range 300K to 3000K, including cloud formation, chemical non-equilibrium effects, and stellar irradiation. The models are called MSG, because they are based on an iterative coupling between three well tested codes, the MARCS stellar atmosphere code, the StaticWeather cloud formation code and the GGchem chemical equilibrium code. It includes up-to-date molecular and atomic opacities, cloud formation and advanced chemical equilibrium calculations, and involves new numerical methods at low temperatures to allow robust convergence. The coupling between the MARCS radiative transfer and GGchem chemical equilibrium computations has made it possibly effectively to reach convergence based on electron pressure for the warmer models and gas pressure for the cooler models, enabling self-consistent modelling of stellar, sub-stellar and exoplanetary objects in a very wide range of effective temperatures. Here we describe the basic details of the models, with illustrative examples of cloudy and irradiated models as well as models based on non-equilibrium chemistry. The qualitative changes in the relative abundances of TiO, H2O, CH4, NH3, and other molecules in our models follow the observationally defined M, L, T (and Y) sequences, but reveal more complex and depth dependent abundance changes, and therefore a spectral classification depending on more parameters. The self consistent coupling to Static-Weather cloud computations, allows detailed comparison between nucleation and observed relative dimming of different spectral bands, with advanced applications for new identification methods of potential exoplanetary biology.
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