Bulk and Atmospheric Metallicities as Direct Probes of Sequentially Varying Accretion Mechanisms of Gas and Solids Onto Planets

Yasuhiro Hasegawa and Mark R. Swain
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Abstract

Core accretion is the standard scenario of planet formation, wherein planets are formed by sequential accretion of gas and solids, and is widely used to interpret exoplanet observations. However, no direct probes of the scenario have been discussed yet. Here, we introduce an onion-like model as one idealization of sequential accretion and propose that bulk and atmospheric metallicities of exoplanets can be used as direct probes of the process. Our analytical calculations, coupled with observational data, demonstrate that the trend of observed exoplanets supports the sequential accretion hypothesis. In particular, accretion of planetesimals that are ≳100 km in size is most favored to consistently explain the observed trends. The importance of opening gaps in both planetesimal and gas disks following planetary growth is also identified. A new classification is proposed, wherein most observed planets are classified into two interior statuses: globally mixed and locally (well) mixed. Explicit identification of the locally (well) mixed status enables reliable verification of sequential accretion. During the JWST era, the quality and volume of observational data will increase drastically and improve exoplanet characterization. This work provides one key reference of how both the bulk and atmospheric metallicities can be used to constrain gas and solid accretion mechanisms of planets.
作为行星上气体和固体依次变化的吸积机制的直接探针的体积和大气金属性
核心吸积是行星形成的标准情景,即行星是由气体和固体依次吸积形成的,这种情景被广泛用于解释系外行星的观测结果。然而,目前还没有讨论过对这种情况的直接探测。在这里,我们引入了一个洋葱状模型作为顺序吸积的理想化模型,并提出系外行星的体积和大气金属性可以作为这一过程的直接探测手段。我们的分析计算与观测数据相结合,证明了观测到的系外行星的趋势支持顺序吸积假说。特别是,大小为≳100 公里的类地行星的吸积最能解释观测到的趋势。此外,还发现了行星增长后在小行星和气体盘中打开缺口的重要性。提出了一种新的分类方法,将大多数观测到的行星分为两种内部状态:全局混合和局部(良好)混合。明确识别局部(良好)混合状态可以可靠地验证顺序增生。在 JWST 时代,观测数据的质量和数量都将急剧增加,从而改善系外行星的特征描述。这项工作为如何利用体积金属性和大气金属性来约束行星的气体和固体吸积机制提供了一个重要参考。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
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