论文标题
通过元素丰度测量来限制巨型系外行星的起源
Constraining the origin of giant exoplanets via elemental abundance measurements
论文作者
论文摘要
近距离巨型行星的起源是行星形成理论中的关键开放问题。两个领先的模型是（i）在外磁盘上形成，然后是迁移和（ii）原位形成。在这项工作中，我们确定了两种地层场景的温暖木星的大气组成。对于各种行星形成位置，行星质量和行星尺寸，我们对地球内部和水冰线的外部进行N体模拟，以估计积聚的重型元素质量和最终行星组成。我们发现，这两个模型有很大差异：迁移的巨型行星的金属度比原位形成的行星高2-14倍。发现折射率和挥发物之间的比率在迁移行星的迁移时高于一个，但对于原位形成的行星的比率低于0.4。我们还确定了这两种形成机制的重元素富集与行星质量之间的截然不同的趋势。虽然发现迁移行星的金属性随着行星质量的降低而增加，但原位形成差不多。我们的研究强调了测量温暖木星大气组成及其与其形成和进化路径的联系的重要性。
The origin of close-in giant planets is a key open question in planet formation theory. The two leading models are (i) formation at the outer disk followed by migration and (ii) in situ formation. In this work we determine the atmospheric composition of warm Jupiters for both formation scenarios. We perform N-body simulations of planetesimal accretion interior and exterior to the water ice-line for various planetary formation locations, planetary masses, and planetesimal sizes to estimate the accreted heavy-element mass and final planetary composition. We find that the two models differ significantly: migrating giant planets have 2-14 times higher metallicities than planets that form in situ. The ratio between refractories and volatiles is found to be above one for migrating planets but below 0.4 for planets that form in situ. We also identify very different trends between heavy-element enrichment and planetary mass for these two formation mechanisms. While the metallicity of migrating planets is found to increase with decreasing planetary mass, it is about constant for in situ formation. Our study highlights the importance of measuring the atmospheric composition of warm Jupiters and its connection to their formation and evolutionary paths.
