The hot Jupiters are close-in extra-solar gas giant planets. Their existence poses two fundamental questions. Why are they so close to their host sun-like stars? Why are their inferred radii significantly larger than theoretical expectations? I will address the first question by introducing a framework that allows for a test of theories of migration that rely upon tidal dissipation taking place inside the planet. For the second, I propose that inflated radii are due to a subtle effect known as thermal tides, which render the hot Jupiters in a perpetual state of asynchronous spin. Persistent tidal dissipation is then responsible for heating the planet at great depth, leaving the planet's equilibrium structure in a perpetual state of inflation.
Followed by wine and cheese in Pupin 1402.