超级地球到超级木星系外行星的结构和演化：I。重元素内部富集
Structure and evolution of super-Earth to super-Jupiter exoplanets: I. heavy element enrichment in the interior
摘要：
我们研究了当前行星模型的不确定性，并量化了它们对行星冷却历史和质量半径关系的影响。这些不确定性包括：（i）用于表征重物质物理性质的各种状态方程之间的差异，（ii）重元素在行星内部的分布，（iii）它们的化学成分和（iv）它们对行星演化的热贡献。我们的模型，其中包括一个气态的H/He信封，固体，无气体类地行星的模型进行比较，以检查冷却和由此产生的半径的气体信封的影响。我们发现，对于大于行星质量20%的重物质的一小部分，重元素在行星内部的分布会显著影响演化，从而影响给定年龄的半径。对于具有大核心质量分数（$\simgr$ 50%）的行星，例如海王星质量的凌日行星GJ 436 b，来自核心的重力和热能对行星冷却历史的贡献是不可忽略的，在1 Gyr之后产生$\sim$ 10%的半径影响。我们表明，目前的质量和半径的大质量行星Hat-P-2b的测定需要至少200 $\mearth$的重物质在内部，在边缘的核心吸积模型目前预测的行星形成。我们表明，如果行星作为大规模的$\sim$ 25 $\mjup$可以形成，改进的核心吸积模型预测，氘是能够燃烧的H/He层以上的核心，即使是大的核心质量为$\sim$ 100 $\mearth$。我们提供了从10 $\mearth$到10 M $_{\rm Jup}$的行星演化模型的广泛网格，具有不同的重元素分数。
英文摘要：
We examine the uncertainties in current planetary models and we quantify their impact on the planet cooling histories and mass-radius relationships. These uncertainties include (i) the differences between the various equations of state used to characterize the heavy material thermodynamical properties, (ii) the distribution of heavy elements within planetary interiors, (iii) their chemical composition and (iv) their thermal contribution to the planet evolution. Our models, which include a gaseous H/He envelope, are compared with models of solid, gasless Earth-like planets in order to examine the impact of a gaseous envelope on the cooling and the resulting radius. We find that for a fraction of heavy material larger than 20% of the planet mass, the distribution of the heavy elements in the planet's interior affects substantially the evolution and thus the radius at a given age. For planets with large core mass fractions ($\simgr$ 50%), such as the Neptune-mass transiting planet GJ436b, the contribution of the gravitational and thermal energy from the core to the planet cooling history is not negligible, yielding a $\sim$ 10% effect on the radius after 1 Gyr. We show that the present mass and radius determinations of the massive planet Hat-P-2b require at least 200 $\mearth$ of heavy material in the interior, at the edge of what is currently predicted by the core-accretion model for planet formation. We show that if planets as massive as $\sim$ 25 $\mjup$ can form, as predicted by improved core-accretion models, deuterium is able to burn in the H/He layers above the core, even for core masses as large as $\sim$ 100 $\mearth$. We provide extensive grids of planetary evolution models from 10 $\mearth$ to 10 M$_{\rm Jup}$, with various fractions of heavy elements.
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