HD 209458 b附近的氢起源
The origin of hydrogen around HD 209458b
摘要：
使用数值模拟，Holmstrom等人（2008）提出了一种合理的替代解释，解释了在HD 209458 b过境期间观察到的莱曼α吸收（Vidal-Madjar等人，2003）。他们的结论是，光靠辐射压无法解释观测结果，还需要一种特殊的恒星风。在这里，我们表明，辐射压力本身实际上可以产生所观察到的高速氢原子。我们还强调，即使恒星风是负责观察到的氢，有足够数量的原子与恒星风进行电荷交换，高能中性原子（ENA）模型也需要从行星大气层的类似幅度的显着逃逸在Vidal-Madjar等人引用。（2003年）的报告。
英文摘要：
Using numerical simulation, Holmstrom et al. (2008) proposed a plausible alternative explanation of the observed Lyman-alpha absorption that was seen during the transit of HD 209458b (Vidal-Madjar et al. 2003). They conclude that radiation pressure alone cannot explain the observations and that a peculiar stellar wind is needed. Here we show that radiation pressure alone can in fact produce the observed high-velocity hydrogen atoms. We also emphasize that even if the stellar wind is responsible for the observed hydrogen, to have a sufficient number of atoms for charge exchange with stellar wind, the energetic neutral atom (ENA) model also needs a significant escape from the planet atmosphere of similar amplitude as quoted in Vidal-Madjar et al.(2003).
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