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Giant planets orbiting main-sequence stars closer than 0.1 AU are called hotJupiters. They interact with their stars affecting their angular momentum.Recent observations provide suggestive evidence of excess angular momentum instars with hot Jupiters in comparison to stars with distant and less massiveplanets. This has been attributed to tidal interaction, but needs to beinvestigated in more detail considering also other possible explanationsbecause in several cases the tidal synchronization time scales are much longerthan the ages of the stars. We select stars harbouring transiting hot Jupitersto study their rotation and find that those with an effective temperaturegreater than 6000 K and a rotation period shorter than 10 days are synchronizedwith the orbital motion of their planets or have a rotation periodapproximately twice that of the planetary orbital period. Stars with aneffective temperature lower than 6000 K and a rotation period longer than 10days show a general trend toward synchronization with increasing effectivetemperature or decreasing orbital period. We propose a model for the angularmomentum evolution of stars with hot Jupiters to interpret these observations.It is based on the hypothesis that a close-in giant planet affects the coronalfield of its host star leading to a topology with predominantly closed fieldlines. Our model can be tested observationally and has relevant consequencesfor the relationship between stellar rotation and close-in giant planets aswell as for the application of gyrochronology to estimate the age ofplanet-hosting stars.

Hot Jupiters and the evolution of stellar angular momentum