3D Modeling of Spectra and Light Curves of Hot Jupiters; A First Approach

TL;DR

This study employs a 3D global circulation model combined with the PHOENIX code to simulate spectra and light curves of hot Jupiters, revealing insights into their atmospheric properties and observational features.

Contribution

It introduces a novel approach integrating GCM and PHOENIX simulations to model 3D spectra and light curves of hot Jupiters, including cloud effects and spectral comparisons.

Findings

PHOENIX simulations explain broad features of observed 8 μm light curves.

The reflection spectrum matches the Spitzer secondary-eclipse depth at 3.6 μm.

Discrepancies at other wavelengths suggest the need for varied metallicities.

Abstract

In this paper, a detailed Global Circulation Model was employed to feed the PHOENIX code to calculate 3D spectra and light curves of hot Jupiters. Cloud free and dusty radiative luxes for the planet HD179949b were modeled to show differences between them. The PHOENIX simulations can explain the broad features of the observed 8 {\mu}m light curves, including the fact that the planet-star flux ratio peaks before the secondary eclipse. The PHOENIX reflection spectrum matches the Spitzer secondary-eclipse depth at 3.6 {\mu}m and underpredicts the eclipse depths at 4.5, 5.8 and 8.0 {\mu}m. These discrepancies result from the chemical composition and provide motivation for incorporating different metallicities in future studies.