Determination of the Interior Structure of Transiting Planets in Multiple-Planet Systems

Details Determination of the Interior Structure of Transiting Planets in Multiple-Planet Systems Determination of the Interior Structure of Transiting Planets in Multiple-Planet Systems

2009-07-28

arxiv.org/abs/0907.5019v1

Astronomy and Astrophysics

Astrophysics

Earth and Planetary Astrophysics

13 pages, 2 figures, submitted to ApJ Letters

Scientific paper

Tidal dissipation within a short-period transiting extrasolar planet perturbed by a companion object can drive orbital evolution of the system to a so-called tidal fixed point, in which the apsidal lines of the transiting planet and its perturber are aligned, and for which variations in the orbital eccentricities of both planet and perturber are damped out. Significant contributions to the apsidal precession rate are made by the secular planet-planet interaction, by general relativity, and by the gravitational quadropole fields created by the transiting planet's tidal and rotational distortions. The fixed-point orbital eccentricity of the inner planet is therefore a strong function of the planet's interior structure. We illustrate these ideas in the specific context of the recently discovered HAT-P-13 exo-planetary system, and show that one can already glean important insights into the physical properties of the inner transiting planet. We present structural models of the planet, which indicate that its observed radius can be maintained for a one-parameter sequence of models that properly vary core mass and tidal energy dissipation in the interior. We use an octopole-order secular theory of the orbital dynamics to derive the dependence of the inner planet's eccentricity, on its tidal Love number. We find that the currently measured eccentricity, implies 0.116 < k2_{b} < 0.425, 0 M_{Earth}

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