论文标题
巨型行星形成模型，对重元素的自洽处理
Giant planet formation models with a self-consistent treatment of the heavy elements
论文作者
论文摘要
我们提出了一个新的数值框架，以建模巨型行星的形成和演变。该代码基于用于恒星天体物理学（MESA）实验的恒星演化工具包模块的进一步开发。该模型包括在行星气态包膜中被假定由水冰制成的积聚的行星/卵石的溶解，并且信封富集对行星生长和内部结构的影响是自s节上计算的。我们将模拟应用于木星，并研究不同重元素和气体积聚率对其形成历史的影响。我们表明，假定的失控气体积聚率显着影响行星半径和光度。可以证实，由于更有效的气体积聚，重元素富集会导致较短的形成时间尺度。我们发现，即使假定低重元素积聚率（寡头政权），乘以重元素浓缩木星的形成时间表也与典型磁盘的寿命兼容。最后，我们提供了地球最内向的重元素轮廓的近似值，从而提供了内部结构与行星生长历史之间的联系。
We present a new numerical framework to model the formation and evolution of giant planets. The code is based on the further development of the stellar evolution toolkit Modules for Experiments in Stellar Astrophysics (MESA). The model includes the dissolution of the accreted planetesimals/pebbles, which are assumed to be made of water ice, in the planetary gaseous envelope, and the effect of envelope enrichment on the planetary growth and internal structure is computed self-consistently. We apply our simulations to Jupiter and investigate the impact of different heavy-element and gas accretion rates on its formation history. We show that the assumed runaway gas accretion rate significantly affect the planetary radius and luminosity. It is confirmed that heavy-element enrichment leads to shorter formation timescales due to more efficient gas accretion. We find that with heavy-element enrichment Jupiter's formation timescale is compatible with typical disks' lifetimes even when assuming a low heavy-element accretion rate (oligarchic regime). Finally, we provide an approximation for the heavy-element profile in the innermost part of the planet, providing a link between the internal structure and the planetary growth history.
