  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.
