盘初始条件如何塑造巨行星的大气成分
How disc initial conditions sculpt the atmospheric composition of giant planets
AI总结：
研究通过模拟盘参数对巨行星大气成分的影响，发现尘埃-气体比是关键因素，而大气成分主要由形成位置决定。
摘要：
先前研究揭示了盘参数（质量、半径、粘性、颗粒破碎速度、尘埃-气体比）对巨行星形成的影响，其中更高质量的盘似乎有利于巨行星形成。然而，不同盘属性如何影响形成中的巨行星组成尚不明确。由于尘埃的内向迁移和蒸发颗粒引起的化学演化，直接通过大气丰度追溯行星形成位置的想法受到质疑。这使得大气丰度与行星形成位置之间的关系变得复杂。我们利用包含颗粒迁移和蒸发效应的行星形成模拟，研究不同盘参数如何影响巨行星的大气组成。我们重点研究大气C/O、C/H、O/H和S/H比值，以探测挥发性物质和难熔物质的示踪剂，从而探讨巨行星的不同吸积路径。我们发现大多数盘参数对气态巨行星的大气丰度影响有限，除了尘埃-气体比，较大的值会导致较高的大气丰度。然而，大气丰度由行星形成位置决定，即使在颗粒迁移和蒸发情景中也是如此。我们的研究表明，富含挥发物的巨行星主要在盘内区形成，其中它们可以吸积大量增强的气体。我们的研究显示，试图通过大气丰度追溯巨行星起源的模拟不需要探测所有盘参数，只要盘参数允许巨行星形成。因此，我们得出结论，观测到的行星组成多样性是其形成位置和迁移历史的直接结果。
英文摘要：
Past studies have revealed the dependency of the disc parameters (mass, radius, viscosity, grain fragmentation velocity, dust-to-gas ratio) on the formation of giant planets, where more massive discs seem beneficial for giant planet formation. It is unclear how the different disc properties influence the composition of forming giant planets. The idea that the atmospheric abundances can trace directly the formation location of planets is put into question, due to the chemical evolution of the disc, caused by inward drifting and evaporating pebbles. This complicates the idea of a relation between atmospheric abundances and planet formation locations. We use planet formation simulations that include the effects of pebble drift and evaporation and investigate how the different disc parameters influence the atmospheric composition of giant planets. We focus on the atmospheric C/O, C/H, O/H and S/H ratios allowing us to probe tracers for volatiles and refractories and thus different accretion pathways of giant planets. We find that most of the disc parameters have only a limited influence on the atmospheric abundances of gas giants, except for the dust-to-gas ratio, where a larger value results in higher atmospheric abundances. However the atmospheric abundances are determined by the planetary formation location, even in the pebble drift and evaporation scenario. Our study suggests that volatile-rich giant exoplanets predominantly form in the inner disc regions, where they can accrete large fractions of vapour-enhanced gas. Our study shows that simulations that try to trace the origin of giant planets via their atmospheric abundances do not have to probe all disc parameters, as long as the disc parameters allow the formation of giant planets. Our study thus suggests that the diversity of observed planetary compositions is a direct consequence of their formation location and migration history.
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