VizieR Online Data Catalog: Dissipation in exoplanet hosts from tidal spin-up (Penev+, 2018)

We selected all of the known transiting planets from the NASA exoplanet archive (http://exoplanetarchive.ipac.caltech.edu/) for which the planet mass exceeds 0.1 M_Jup, the orbital period is shorter than 3.5 days, and the star has an effective temperature below 6100 K. The effective temperature cut-off ensures that only stars with surface convective zones are included in the analysis. We decided to focus on these "cool" stars because both theoretical expectations and observations suggest the dominant tidal dissipation mechanism, and hence its efficiency, is dramatically different for stars without a significant surface convective zone. The restrictions on planet mass and orbital period were designed to select systems with strong tides, for which the host stars are most likely to have been measurably spun up. This resulted in an initial sample of 188 systems. Of the 188 systems in the sample, our procedure led to two-sided limits on Q_*' for 35 systems. In another 40 cases, it was possible to derive a lower bound on Q_*'. In the remaining cases, the data did not lead to meaningful constraints. Table 1 summarizes the quantitative results for each system.

(1 data file).