Can Planets Survive Stellar Evolution?
Can Planets Survive Stellar Evolution?
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DOI：
10.1086/516746
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发表时间：
2007-02
期刊：
影响因子：
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通讯作者：
E. Villaver;M. Livio
中科院分区：
文献类型：
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作者：
E. Villaver;M. Livio
我们研究的生存气体行星周围的恒星质量在1-5 M的范围内，因为这些恒星演变的主要序列。我们发现，如果最初位于轨道距离小于3-5 Au，质量小于一个木星质量的行星不会生存的行星状星云阶段。在低质量恒星（主序星为1 M）周围，质量超过2个木星质量的行星在行星状星云阶段幸存下来，轨道距离约为3 Au。当星星经过行星状星云阶段时，蒸发外流将在行星表面形成。蒸发的行星可以通过光谱观测来探测。质量为MWD <$0.7 M的白色周围的行星通常预计会在轨道半径r <$15 Au处被发现。如果在大质量白色矮星周围的较小轨道半径处发现气体行星，它们必须是两颗白色矮星合并的结果。
We study the survival of gas planets around stars with masses in the range 1-5 M☉, as these stars evolve off the main sequence. We show that planets with masses smaller than one Jupiter mass do not survive the planetary nebula phase if located initially at orbital distances smaller than 3-5 AU. Planets more massive than two Jupiter masses around low-mass (1 M☉ on the main sequence) stars survive the planetary nebula stage down to orbital distances of ~3 AU. As the star evolves through the planetary nebula phase, an evaporation outflow will be established at the planet's surface. Evaporating planets may be detected using spectroscopic observations. Planets around white dwarfs with masses MWD ≳ 0.7 M☉ are generally expected to be found at orbital radii r ≳ 15 AU. If gas planets are found at smaller orbital radii around massive white dwarfs, they had to form as the result of the merger of two white dwarfs.