  Understanding the anomalous radii of many transiting hot gas giant planets is
a fundamental problem of planetary science. Recent detections of re-inflated
warm Jupiters orbiting post-main-sequence stars and the re-inflation of hot
Jupiters while their host stars evolve on the main-sequence may help constrain
models for the anomalous radii of hot Jupiters. In this work, we present
evolution models studying the re-inflation of gas giants to determine how
varying the depth and intensity of deposited heating affects both main-sequence
re-inflation of hot Jupiters and post-main-sequence re-inflation of warm
Jupiters. We find that deeper heating is required to re-inflate hot Jupiters
than is needed to suppress their cooling, and that the timescale of
re-inflation decreases with increasing heating rate and depth. We find a strong
degeneracy between heating rate and depth, with either strong shallow heating
or weak deep heating providing an explanation for main-sequence re-inflation of
hot Jupiters. This degeneracy between heating rate and depth can be broken in
the case of post-main-sequence re-inflation of warm Jupiters, as the inflation
must be rapid to occur within post-main-sequence evolution timescales. We also
show that the dependence of heating rate on incident stellar flux inferred from
the sample of hot Jupiters can explain re-inflation of both warm and hot
Jupiters. TESS will obtain a large sample of warm Jupiters orbiting
post-main-sequence stars, which will help to constrain the mechanism(s) causing
the anomalous radii of gas giant planets.
