THE EVOLUTION OF STELLAR ROTATION AND THE HYDROGEN ATMOSPHERES OF HABITABLE-ZONE TERRESTRIAL PLANETS
THE EVOLUTION OF STELLAR ROTATION AND THE HYDROGEN ATMOSPHERES OF HABITABLE-ZONE TERRESTRIAL PLANETS
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DOI：
10.1088/2041-8205/815/1/l12
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发表时间：
2015-11
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影响因子：
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通讯作者：
C. Johnstone;M. Güdel;A. Stökl;H. Lammer;L. Tu;K. Kislyakova;T. Lüftinger;P. Odert;N. Erkaev;E. Dorfi
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作者：
C. Johnstone;M. Güdel;A. Stökl;H. Lammer;L. Tu;K. Kislyakova;T. Lüftinger;P. Odert;N. Erkaev;E. Dorfi
在气态原行星盘中形成的类地行星可以积累大量的氢气包层。由于XUV驱动的蒸发导致的这种大气的演化取决于主星的活动演化，而主星本身又敏感地依赖于它的自转演化，因此也取决于它的初始自转速度。在这封信中，我们导出了一种简单实用的计算行星大气蒸发的方法，该方法结合了流体静力低层大气和流体动力高层大气的模型。我们发现，中心恒星的初始自转速度对于行星大气的演化至关重要，并可以决定行星是否保留或失去其原始氢包层。我们的结果强调了在研究行星大气的演化时，需要对恒星活动演化进行详细的处理。
Terrestrial planets formed within gaseous protoplanetary disks can accumulate significant hydrogen envelopes. The evolution of such an atmosphere due to XUV driven evaporation depends on the activity evolution of the host star, which itself depends sensitively on its rotational evolution, and therefore on its initial rotation rate. In this Letter, we derive an easily applicable method for calculating planetary atmosphere evaporation that combines models for a hydrostatic lower atmosphere and a hydrodynamic upper atmosphere. We show that the initial rotation rate of the central star is of critical importance for the evolution of planetary atmospheres and can determine if a planet keeps or loses its primordial hydrogen envelope. Our results highlight the need for a detailed treatment of stellar activity evolution when studying the evolution of planetary atmospheres.