The Effects of Irradiation on Hot Jovian Atmospheres: Heat Redistribution and Energy Dissipation

TL;DR

This study uses 3D models to analyze how irradiation affects heat redistribution, atmospheric dynamics, and energy dissipation in hot Jupiter atmospheres, revealing key dependencies on irradiation levels and temperature inversions.

Contribution

It provides new insights into the effects of irradiation and temperature inversions on heat redistribution, atmospheric flow, and energy dissipation mechanisms in hot Jupiters.

Findings

Heat redistribution is efficient at T bc 2000 K, leading to similar day and night fluxes.

High irradiation levels cause breakdown of heat redistribution, increasing day-night flux contrast.

Ohmic dissipation occurs deeper and increases with irradiation, potentially causing radius inflation.

Abstract

Hot Jupiters, due to the proximity to their parent stars, are subjected to a strong irradiating flux which governs their radiative and dynamical properties. We compute a suite of 3D circulation models with dual-band radiative transfer, exploring a relevant range of irradiation temperatures, both with and without temperature inversions. We find that, for irradiation temperatures T \lesssim 2000 K, heat redistribution is very efficient, producing comparable day- and night-side fluxes. For Tirr \approx 2200-2400 K, the redistribution starts to break down, resulting in a high day-night flux contrast. Our simulations indicate that the efficiency of redistribution is primarily governed by the ratio of advective to radiative timescales. Models with temperature inversions display a higher day-night contrast due to the deposition of starlight at higher altitudes, but we find this opacity-driven effect to be secondary compared to the effects of irradiation. The hotspot offset from the substellar point is large when insolation is weak and redistribution is efficient, and decreases as redistribution breaks down. The atmospheric flow can be potentially subjected to the Kelvin-Helmholtz instability (as indicated by the Richardson number) only in the uppermost layers, with a depth that penetrates down to pressures of a few millibars at most. Shocks penetrate deeper, down to several bars in the hottest model. Ohmic dissipation generally occurs down to deeper levels than shock dissipation (to tens of bars), but the penetration depth varies with the atmospheric opacity. The total dissipated Ohmic power increases steeply with the strength of the irradiating flux and the dissipation depth recedes into the atmosphere, favoring radius inflation in the most irradiated objects.