Diurnal Thermal Tides in a Non-synchronized Hot Jupiter

Abstract

We perform a linear analysis to investigate the dynamical response of a non-synchronized hot Jupiter to stellar irradiation. In this work, we consider the diurnal Fourier harmonic of the stellar irradiation acting at the top of a radiative layer of a hot Jupiter with no clouds and winds. In the absence of the Coriolis force, the diurnal thermal forcing can excite internal waves propagating into the planet's interior when the thermal forcing period is longer than the sound crossing time of the planet's surface. When the Coriolis effect is taken into consideration, the latitude-dependent stellar heating can excite weak internal waves (g modes) and/or strong baroclinic Rossby waves (buoyant r modes) depending on the asynchrony of the planet. When the planet spins faster than its orbital motion (i.e. retrograde thermal forcing), these waves carry negative angular momentum and are damped by radiative loss as they propagate downwards from the upper layer of the radiative zone. As a result, angular momentum is transferred from the lower layer of the radiative zone to the upper layer and generates a vertical shear. We estimate the resulting internal torques for different rotation periods based on the parameters of HD 209458b.

accepted for publication in MNRAS

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• 3D Structures of equatorial waves and the resulting superrotation in the atmosphere of a tidally locked hot Jupiter
• A Significant Increase in Detection of High-Resolution Emission Spectra Using a Three-Dimensional Atmospheric Model of a Hot Jupiter
• BEER analysis of Kepler and CoRoT light curves: II. Evidence for superrotation in the phase curves of three Kepler hot Jupiters
• Gravity Waves on Hot Extrasolar Planets: I. Propagation and Interaction with the Background
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• Semidiurnal thermal tides in asynchronously rotating hot Jupiters
• Modeling the Thermal Bulge of A Hot Jupiter with the Two-Stream Approximation
• The generalized non-conservative model of a 1-planet system - revisited
• Thermally Driven Angular Momentum Transport in Hot Jupiters