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Some transiting extrasolar giant planets have measured radii larger thanpredicted by the standard theory. In this paper, we explore the possibilitythat an earlier episode of tidal heating can explain such radius anomalies andapply the formalism we develop to HD 209458b as an example. We find that forstrong enough tides the planet's radius can undergo a transient phase ofinflation that temporarily interrupts canonical, monotonic shrinking due toradiative losses. Importantly, an earlier episode of tidal heating can resultin a planet with an inflated radius, even though its orbit has nearlycircularized. Moreover, we confirm that at late times, and under somecircumstances, by raising tides on the star itself a planet can spiral into itshost. We note that a 3$\times$ to 10$\times$solar planet atmospheric opacitywith no tidal heating is sufficient to explain the observed radius of HD209458b. However, our model demonstrates that with an earlier phase of episodictidal heating we can fit the observed radius of HD 209458b even with lower(solar) atmospheric opacities. This work demonstrates that, if a planet is leftwith an appreciable eccentricity after early inward migration and/or dynamicalinteraction, coupling radius and orbit evolution in a consistent fashion thatincludes tidal heating, stellar irradiation, and detailed model atmospheresmight offer a generic solution to the inflated radius puzzle for transitingextrasolar giant planets such as WASP-12b, TrES-4, and WASP-6b.

Coupled Evolution with Tides of the Radius and Orbit of Transiting Giant Planets: General Results