  We study the interaction between stellar irradiation and tidal heating in
gaseous planets with short orbital periods. The intentionally simplified
atmospheric model we employ makes the problem analytically tractable and
permits the derivation of useful scaling relations. We show that many tidal
models provide thermal feedback, producing interior radiative zones and leading
to enhanced g-mode dissipation with a wide spectrum of resonances. These
resonances are dynamically tuned by the thermal feedback, and so represent a
novel form of thermomechanical feedback, coupling vibrational modes to the very
slow thermal evolution of the planet. We then show that stellar irradiation
allows the heat produced by these modes to be trapped at depth with high
efficiency, leading to entropy increase in the central convective region, as
well as expansion of the planet's radius sufficient to match observed swelling.
We find that thermally driven winds play an essential role in this process by
making the thermal structure of the atmosphere spherically symmetric within a
few scale heights of the photosphere. We characterise the relationship between
the swelling factor, the orbital period and the host star and determine the
timescale for swelling. We show that these g-modes suffice to produce bloating
on the order of the radius of the planet over $\mathrm{Gyr}$ timescales when
combined with significant insolation and we provide analytic relations for the
relative magnitudes of tidal heating and insolation.
