论文标题
系外行星中的双峰分布：考虑不同的核心成分和$ \ rm h_ {2} $信封的尺寸
The Bimodal Distribution in Exoplanet Radii: Considering Varying Core Compositions and $\rm H_{2}$ Envelope's Sizes
论文作者
论文摘要
引入了几种模型，以解释Fulton等人观察到的系外行星半径中的半径分布。 （2017）一个峰值为$ \ rm \ sim \ sim 1.3 r _ {\ oplus} $ th $ \ rm \ rm \ sim 2.4 r _ {\ oplus} $，最小值为$ \ rm \ rm \ sim 1.75r _ {\ oplus} $。在本文中，我们重点介绍了外部球星大小分布是由XUV引起的大气损失引起的。我们通过将合成ZAMS恒星的XUV辐照暴露于XUV辐照中，从而进化了$ 10^{6} $合成系外行星。对于每个星球，我们设置了不同的内部成分，范围从$ \ rm 100 \：wt \％$ fe（非常致密）到$ \ rm \ rm 100 \：wt \％$ $ $ $ \ rm mgsio_ {3} $（平均密度）（平均密度）和$ \ $ \ \ wt \：wt \ wt \％$ $ $ $ $ $ $ \ rm h_信封尺寸从$ \ rm 0 \：wt \％$（可忽略的信封）到$ \ rm 100 \：wt \％$（可忽略的核心）。我们的模拟能够复制系外行星中的双峰分布。我们认为，为了重现Fulton等人的分布。 （2017年）必须有一个超过$ \ rm \ sim \ sim 8m _ {\ oplus} $的质量的系外行星。此外，我们的最佳拟合结果可以预测，$ \ rm m_ {p} \ lyseSim 8M _ {\ oplus} $的外部外部发行的初始平坦分布，并且具有$ \ rm \ rm \ rmsim 3m _ {\ oplus} $的行星的强烈不足。我们的结果与$ \ rm \ sim 1.3r _ {\ oplus} $ radius Peak主要包含裸露的外部球星，而$ \ rm \ rm \ sim 2.4r _ {\ oplus}
Several models have been introduced in order to explain the radius distribution in exoplanet radii observed by Fulton et al. (2017) with one peak at $\rm \sim 1.3 R_{\oplus} $ the other at $\rm \sim 2.4 R_{\oplus} $ and the minimum at $\rm \sim 1.75R_{\oplus} $. In this paper we focus on the hypothesis that the exoplanet size distribution is caused by stellar XUV-induced atmospheric loss. We evolve $10^{6}$ synthetic exoplanets by exposing them to XUV irradiation from synthetic ZAMS stars. For each planet we set a different interior composition which ranged from $\rm 100 \: wt\%$ Fe (very dense) through $\rm 100 \: wt\%$ $\rm MgSiO_{3}$ (average density) and to $\rm 100 \: wt\%$ $\rm H_{2}O$ ice (low density) with varying hydrogen envelop sizes which varied from $\rm 0 \: wt\%$ (a negligible envelop) to $\rm 100 \: wt\%$ (a negligible core). Our simulations were able to replicate the bimodal distribution in exoplanet radii. We argue that in order to reproduce the distribution by Fulton et al. (2017) it is mandatory for there to be a paucity of exoplanets with masses above $\rm \sim 8M_{\oplus}$. Furthermore, our best-fit result predicts an initial flat distribution in exoplanet occurrence for $\rm M_{P} \lesssim 8M_{\oplus}$ with a strong deficiency for planets with $\rm \lesssim 3M_{\oplus}$. Our results are consistent with the $\rm \sim 1.3R_{\oplus}$ radius peak mostly encompassing denuded exoplanets whilst the $\rm \sim 2.4R_{\oplus}$ radius peak mainly comprising exoplanets with large hydrogen envelops
