由极紫外光离加热驱动的大气逸出的物理学:近地行星流体动力学逸出的分类

Hiroto Mitani, Riouhei Nakatani, N. Yoshida
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引用次数: 0

摘要

强烈的极紫外辐射加热近地系外行星的上层大气,驱动大气逃逸。逃逸过程决定了近地行星的行星演化。质量损失率取决于行星上的紫外线通量。我们介绍了描述大气中主要物理性质的相关物理量。我们发现平衡温度和特征温度决定了系统是能量受限还是重组受限。我们用物理条件对观测到的近地行星进行分类。我们还发现,许多探测到莱曼α吸收的行星接收的通量比可由物理条件确定的临界通量更强。我们的分类方法可以定量地揭示EUV是否不足以驱动流出,或者由于某些原因(如恒星风限制)没有检测到莱曼α吸收。我们还讨论了水动力模拟的热化学结构与相关物理。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Physics of the atmospheric escape driven by EUV photoionization heating: Classification of the hydrodynamic escape in close-in planets
Abstract The intense extreme ultraviolet radiation heats the upper atmosphere of close-in exoplanets and drives the atmospheric escape. The escaping process determines the planetary evolution of close-in planets. The mass loss rate depends on the UV flux at the planet. We introduce the relevant physical quantities which describe the dominant physics in the atmosphere. We find that the equilibrium temperature and the characteristic temperature determine whether the system becomes energy-limited or recombination-limited. We classify the observed close-in planets using the physical conditions. We also find that many of the Lyman-α absorptions detected planets receive intenser flux than the critical flux which can be determined from physical conditions. Our classification method can quantitatively reveal whether the EUV is not strong enough to drive the outflow or the Lyman- α absorption is not detected for some reason (e.g. stellar wind confinement). We also discuss the thermo-chemical structure of hydrodynamic simulations with the relevant physics.
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