各种质量恒星周围的行星形成：雪线和巨行星的频率
Planet formation around stars of various masses: The snow line and the frequency of giant planets
摘要：
我们使用一个半解析的星周盘模型，认为雪线通过吸积和中心恒星的演化运动，研究气体巨星的频率如何随恒星质量的变化。雪线距离随恒星质量的变化很小，因此巨行星的光谱类型范围很广。在0.4 ~ 3 M太阳质量范围内，一颗恒星至少存在一颗气体巨星的概率随恒星质量的增加而线性增加。质量大于3M_sun的恒星迅速向主序星演化，在原行星形成之前，将雪线推到10-15 AU，并限制了形成巨行星核的盘质量范围。如果太阳质量恒星周围气体巨星的出现频率为6%，则0.4M太阳恒星的出现率为1%，1.5M太阳恒星的出现率为10%。这个结果对我们假设的模型参数很不敏感。最后，当大于2.5M太阳的恒星向主序星移动时，雪线的移动可能允许Leger等人提出的海洋行星。#21453;，不迁移。
英文摘要：
We use a semi-analytic circumstellar disk model that considers movement of the snow line through evolution of accretion and the central star to investigate how gas giant frequency changes with stellar mass. The snow line distance changes weakly with stellar mass; thus giant planets form over a wide range of spectral types. The probability that a given star has at least one gas giant increases linearly with stellar mass from 0.4 M_sun to 3 M_sun. Stars more massive than 3 M_sun evolve quickly to the main-sequence, which pushes the snow line to 10-15 AU before protoplanets form and limits the range of disk masses that form giant planet cores. If the frequency of gas giants around solar-mass stars is 6%, we predict occurrence rates of 1% for 0.4 M_sun stars and 10% for 1.5 M_sun stars. This result is largely insensitive to our assumed model parameters. Finally, the movement of the snow line as stars >2.5 M_sun move to the main-sequence may allow the ocean planets suggested by Leger et. al. to form without migration.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
