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The multiple-planet systems discovered by the Kepler mission show an excessof planet pairs with period ratios just wide of exact commensurability forfirst-order resonances like 2:1 and 3:2. In principle, these planet pairs couldhave both resonance angles associated with the resonance librating if theorbital eccentricities are sufficiently small, because the width of first-orderresonances diverges in the limit of vanishingly small eccentricity. We considera widely-held scenario in which pairs of planets were captured into first-orderresonances by migration due to planet-disk interactions, and subsequentlybecame 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 theplanet's tidal dissipation function and Love number that implies that some ofthe Kepler planets are likely solid. However, tides are not strong enough tomove many of the planet pairs to the observed separations, suggesting thatadditional dissipative processes are at play.

Are the Kepler Near-Resonance Planet Pairs due to Tidal Dissipation?