期刊
ASTROPHYSICAL JOURNAL
卷 568, 期 2, 页码 L117-L120出版社
IOP PUBLISHING LTD
DOI: 10.1086/339794
关键词
celestial mechanics; planetary systems; solar system : formation; solar system : general; stars : individual (HD 82943, HD 179949, tau Bootis, nu Andromedae); stars : rotation; stellar dynamics
About 68 extrasolar planets around main-sequence stars of spectral types F, G, and K have been discovered up to now. The minimum masses (M-p sin i) of these planets are ranging from fractions of a Jupiter mass (M-J) to 15 M-J. The semimajor axes of the planetary orbits range from 0.04 out to 4 AU. At large semimajor axes, only massive planets have been discovered because of observational selection effects. For semimajor axes less than 0.1 AU, however, there seems to be an observational lack of very massive planets (>1 M-J). Here we explain the absence of massive planets at these distances by tidal interactions between planets and their central star that lead to a rapid decay of a planetary orbit toward the Roche zone of the star within a short timescale. A higher metallicity of planet-bearing stars and the recent discovery of a Li-6 excess of a G0 star might further indicate that planets can indeed get lost in their host stars.
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据