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We study the tidal response of rotating solar mass stars, as well as moremassive rotating stars, of different ages in the context of tidal capturesleading to either giant exoplanets on close in orbits, or the formation ofbinary systems in star clusters. To do this, we adopt approaches based onnormal mode and associated overlap integral evaluation, developed in acompanion paper by Ivanov et al., and direct numerical simulation, to evaluateenergy and angular momentum exchanges between the orbit and normal modes. Thetwo approaches are found to be in essential agreement apart from whenencounters occur near to pseudosynchronization, where the stellar angularvelocity and the orbital angular velocity at periastron are approximatelymatched. We find that the strength of tidal interaction being expressed indimensionless natural units is significantly weaker for the more massive stars,as compared to the solar mass stars, because of the lack of significantconvective regions in the former case. On the other hand the interaction isfound to be stronger for retrograde as opposed to prograde orbits in all cases.In addition, for a given pericentre distance, tidal interactions alsostrengthen for more evolved stars on account of their radial expansion. Inagreement with previous work based on simplified polytropic models, we findthat energy transferred to their central stars could play a significant role inthe early stages of the circularisation of potential 'Hot Jupiters'.

Dynamical tides excited in rotating stars of different masses and ages and the formation of close in orbits