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Evidence for Solid Planets from Kepler's Near-Resonance Systems

Published online by Cambridge University Press:  29 April 2014

Man Hoi Lee ,
D. Fabrycky  and
D. N. C. Lin
Man Hoi Lee
Affiliation:
Dept. of Earth Sciences and Dept. of Physics, The University of Hong Kong, Hong Kong
D. Fabrycky
Affiliation:
Dept. of Astronomy & Astrophysics, University of Chicago, 5640 S. Ellis Ave., Chicago, IL 60637, USA UCO/Lick Observatory, University of California, Santa Cruz, CA 95064, USA
D. N. C. Lin
Affiliation:
UCO/Lick Observatory, University of California, Santa Cruz, CA 95064, USA
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Abstract

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The multiple-planet systems discovered by the Kepler mission show an excess of planet pairs with period ratios just wide of exact commensurability for first-order resonances like 2:1 and 3:2. In principle, these planet pairs could be in resonance if their orbital eccentricities are sufficiently small, because the width of first-order resonances diverges in the limit of vanishingly small eccentricity. We consider a widely-held scenario in which pairs of planets were captured into first-order resonances by migration due to planet-disk interactions, and subsequently became detached from the resonances, due to tidal dissipation in the planets. In the context of this scenario, we find a constraint on the ratio of the planet's tidal dissipation function and Love number that implies that some of the Kepler planets are likely solid. However, tides are not strong enough to move many of the planet pairs to the observed separations, suggesting that additional processes are at play.

Keywords

celestial mechanicssolar system: formationplanetary systems: formation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S293: Formation, Detection, and Characterization of Extrasolar Habitable Planets , August 2012 , pp. 100 - 105
Copyright
Copyright © International Astronomical Union 2014 

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