Measuring Tidal Dissipation in Giant Planets from Tidal Circularization

Abstract

In this project, we determined the constraints on the modified tidal quality factor, $Q_{pl}^{\prime }$, of gas-giant planets orbiting close to their host stars. We allowed $Q_{pl}^{\prime }$ to depend on tidal frequency, accounting for the multiple tidal waves with time-dependent frequencies simultaneously present on the planet. We performed our analysis on 78 single-star and single-planet systems, with giant planets and host stars with radiative cores and convective outer shells. We extracted constraints on the frequency-dependent $Q_{pl}^{\prime }$ for each system separately and combined them to find general constraints on $Q_{pl}^{\prime }$ required to explain the observed eccentricity envelope while simultaneously allowing the observed eccentricities of all systems to survive to the present day. Individual systems do not place tight constraints on $Q_{pl}^{\prime }$. However, since similar planets must have similar tidal dissipation, we require that a consistent, possibly frequency-dependent, model must apply. Under that assumption, we find that the value of ${\log }_{10}{Q}_{pl}^{\prime }$ for HJs is $5.0\pm 0.5$ for the range of tidal period from 0.8 to 7 days. We did not see any clear sign of frequency dependence of $Q_{pl}^{\prime }$.

Accepted for publication in MNRAS 19 pages, 11 figures, 2 tables

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