ORBITAL DECAY OF HOT JUPITERS DUE TO NONLINEAR TIDAL DISSIPATION WITHIN SOLAR-TYPE HOSTS

被引：85

作者：

Essick, Reed ^{[1
]}

Weinberg, Nevin N.

机构：

[1] MIT, Dept Phys, Cambridge, MA 02139 USA

来源：

ASTROPHYSICAL JOURNAL | 2016年 / 816卷 / 01期

基金：

美国国家科学基金会;

关键词：

gravitation; instabilities; planets and satellites: dynamical evolution and stability; waves; INTERNAL WAVE BREAKING; IN EXTRASOLAR PLANETS; GIANT PLANETS; STARS; EVOLUTION; EXOPLANETS; DESTRUCTION; GRAVITY; OSCILLATIONS; INSTABILITY;

D O I：

10.3847/0004-637X/816/1/18

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We study the orbital evolution of hot Jupiters due to the excitation and damping of tidally driven g-modes within solar-type host stars. Linearly resonant g-modes (the dynamical tide) are driven to such large amplitudes in the stellar core that they excite a sea of other g-modes through weakly nonlinear interactions. By solving the dynamics of large networks of nonlinearly coupled modes, we show that the nonlinear dissipation rate of the dynamical tide is several orders of magnitude larger than the linear dissipation rate. We find stellar tidal quality factors Q(*)' similar or equal to 10(5)-10(6) for systems with planet mass M-p greater than or similar to 0.5M(J) and orbital period P less than or similar to 2 days, which implies that such systems decay on timescales that are small compared to the main-sequence lifetime of their solar-type hosts. According to our results, there are similar or equal to 10 currently known exoplanetary systems, including WASP-19b and HAT-P-36-b, with orbital decay timescales shorter than a Gyr. Rapid, tidally induced orbital decay may explain the observed paucity of planets with M-p greater than or similar to M-J and P < 2 days around solar-type hosts and could generate detectable transit-timing variations in the near future.

引用

页数：21

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