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Context. With the detection of thousands of exoplanets, characterising theirdynamical evolution in detail represents a key step in the understanding oftheir formation. Studying the dissipation of tides occurring both in the hoststar and in the planets is of great relevance in order to investigate thedistribution of the angular momentum occurring among the objects populating thesystem and to studying the evolution of the orbital parameters. From atheoretical point of view, the dissipation of tides throughout a body may bestudied by relying on the so-called phase or time-lag equilibrium tides modelin which the reduced tidal quality factor Q'p, or equivalently the productbetween the love number and the time lag (k2DeltaT), describe how efficientlytides are dissipated within the perturbed body. Constraining these factors bylooking at the current configuration of the exoplanetary system is extremelychallenging, and simulations accounting for the evolution of the system as awhole might help to shed some light on the mechanisms governing this process.Aims. We aim to constrain the tidal dissipation factors of hot-Jupiter-likeplanets by studying the orbital evolution of Kepler-91b. Methods. We firstlycarried out a detailed asteroseismc characterisation of Kepler-91 and computeda dedicated stellar model using both classical and astereoseismic constraints.We then coupled the evolution of the star to the one of the planets by means ofour orbital evolution code and studied the evolution of the system byaccounting for tides dissipated both in the planet and in the host star.Results. We found that the maximum value for k2DeltaT (or equivalently theminimum value for Q'p) determining the efficiency of equilibrium tidesdissipation occurring within Kepler-91b is 0.4 pm 0.25 s (4.5+5.8 * 10^5).

Constraints on planetary tidal dissipation from a detailed study of Kepler 91b