GASTLI：一个开源的内部分层-大气耦合模型，用于揭示气态巨行星的组成
GASTLI: An open-source coupled interior-atmosphere model to unveil gas giant composition
AI总结：
本文推出开源Python包GASTLI，通过耦合内部结构与无云大气模型快速计算气态巨行星的质量-半径关系和热演化，并在太阳系巨行星及HAT-P-26 b上验证其可靠性，揭示不同状态方程对金属质量分数估计的影响。
摘要：
气态巨行星的金属质量分数是约束其形成机制和演化的有力工具。金属含量是通过将质量和半径测量值与内部结构和演化模型进行比较来推断的。在JWST、CHEOPS、TESS以及即将到来的PLATO时代，我们即将在半径、年龄和大气金属丰度测量方面获得前所未有的精度。为了迎接这一丰富的数据，我们推出了GAS gianT modeL for Interiors（GASTLI），这是一个易于使用、公开可用的Python软件包。该代码经过优化，能够快速计算各种包层组成和核心质量分数下的质量-半径关系，以及半径和光度的热演化曲线。其适用范围包括质量为17 M⊕ < M < 6 MJup、平衡温度Teq < 1000 K的行星。内部模型分层为由水和岩石组成的核心，以及由H/He和金属（水）构成的包层。内部与一个自洽、无云的大气模型网格耦合，以确定大气和边界内部温度，以及大气对总半径的贡献。我们通过将GASTLI与先前的工作以及太阳系气态巨行星和海王星的数据进行比较，成功验证了该模型。我们还在海王星质量系外行星HAT-P-26 b上测试了GASTLI，发现其整体金属质量分数在0.60-0.78之间，核心质量为8.5-14.4 M⊕。最后，我们探讨了不同状态方程和假设（如C/O比和凌日压力）对整体金属质量分数估计的影响。内部模型之间的这些差异导致木星质量行星的半径变化高达2.5%，而海王星质量行星的半径变化超过10%。这相当于核心质量分数变化0.07，或包层金属质量分数变化0.10。
英文摘要：
The metal mass fractions of gas giants are a powerful tool to constrain their formation mechanisms and evolution. The metal content is inferred by comparing mass and radius measurements with interior structure and evolution models. In the midst of the JWST, CHEOPS, TESS, and the forthcoming PLATO era, we are at the brink of obtaining unprecedented precision in radius, age and atmospheric metallicity measurements. To prepare for this wealth of data, we present the GAS gianT modeL for Interiors (GASTLI), an easy-to-use, publicly available Python package. The code is optimized to rapidly calculate mass-radius relations, and radius and luminosity thermal evolution curves for a variety of envelope compositions and core mass fractions. Its applicability spans planets with masses $17 \ M_{\oplus} < M < 6 \ M_{Jup}$, and equilibrium temperatures $T_{eq} < 1000$ K. The interior model is stratified in a core composed of water and rock, and an envelope constituted by H/He and metals (water). The interior is coupled to a grid of self-consistent, cloud-free atmospheric models to determine the atmospheric and boundary interior temperature, as well as the contribution of the atmosphere to the total radius. We successfully validate GASTLI by comparing it to previous work and data of the Solar System's gas giants and Neptune. We also test GASTLI on the Neptune-mass exoplanet HAT-P-26 b, finding a bulk metal mass fraction between 0.60-0.78 and a core mass of 8.5-14.4 $M_{\oplus}$. Finally, we explore the impact of different equations of state and assumptions, such as C/O ratio and transit pressure, in the estimation of bulk metal mass fraction. These differences between interior models entail a change in radius of up to 2.5% for Jupiter-mass planets, but more than 10\% for Neptune-mass. These are equivalent to variations in core mass fraction of 0.07, or 0.10 in envelope metal mass fraction.
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