2018MNRAS.476.2542C

Transiting hot Jupiters occupy a wedge-shaped region in the mass ratio-orbital separation diagram. Its upper boundary is eroded by tidal spiral-in of massive, close-in planets and is sensitive to the stellar tidal dissipation parameter Q_ s_^′. We develop a simple generative model of the orbital separation distribution of the known population of transiting hot Jupiters, subject to tidal orbital decay, XUV-driven evaporation and observational selection bias. From the joint likelihood of the observed orbital separations of hot Jupiters discovered in ground-based wide-field transit surveys, measured with respect to the hyperparameters of the underlying population model, we recover narrow posterior probability distributions for Q_ s_^′ in two different tidal forcing frequency regimes. We validate the method using mock samples of transiting planets with known tidal parameters. We find that Q_ s_^′ and its temperature dependence are retrieved reliably over five orders of magnitude in Q_ s_^′. A large sample of hot Jupiters from small-aperture ground-based surveys yields log₁₀ Q_ s_^′^=(8.26±0.14) for 223 systems in the equilibrium-tide regime. We detect no significant dependence of Q_ s_^′ on stellar effective temperature. A further 19 systems in the dynamical-tide regime yield log₁₀ Q_ s_^′^=7.3±0.4, indicating stronger coupling. Detection probabilities for transiting planets at a given orbital separation scale inversely with the increase in their tidal migration rates since birth. The resulting bias towards younger systems explains why the surface gravities of hot Jupiters correlate with their host stars' chromospheric emission fluxes. We predict departures from a linear transit-timing ephemeris of less than 4 s for WASP-18 over a 20-yr baseline.