Tidal Decay of Close Planetary Orbits

Details Tidal Decay of Close Planetary Orbits Tidal Decay of Close Planetary Orbits

1996-05-11

arxiv.org/abs/astro-ph/9605059v1

Astronomy and Astrophysics

Astrophysics

AAS LaTeX macros v.4, 14 pages, 2 postscript figures, also available from http://ensor.mit.edu/~rasio/, to appear in ApJ

Scientific paper

10.1086/177941

The 4.2-day orbit of the newly discovered planet around 51~Pegasi is formally unstable to tidal dissipation. However, the orbital decay time in this system is longer than the main-sequence lifetime of the central star. Given our best current understanding of tidal interactions, a planet of Jupiter's mass around a solar-like star could have dynamically survived in an orbit with a period as short as $\sim10\,$hr. Since radial velocities increase with decreasing period, we would expect to find those planets close to the tidal limit first and, unless this is a very unusual system, we would expect to find many more. We also consider the tidal stability of planets around more evolved stars and we re-examine in particular the question of whether the Earth can dynamically survive the red-giant phase in the evolution of the Sun.

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