  The energy deposition and redistribution in hot Jupiter atmospheres is not
well understood currently, but is a major factor for their evolution and
survival. We present a time dependent radiative transfer model for the
atmosphere of WASP-18b which is a massive (10 MJup) hot Jupiter (Teq ~ 2400 K)
exoplanet orbiting an F6V star with an orbital period of only 0.94 days. Our
model includes a simplified parametrisation of the day-to-night energy
redistribution by a modulation of the stellar heating mimicking a solid body
rotation of the atmosphere. We present the cases with either no rotation at all
with respect to the synchronously rotating reference frame or a fast
differential rotation. The results of the model are compared to previous
observations of secondary eclipses of Nymeyer et al. (2011) with the Spitzer
Space Telescope. Their observed planetary flux suggests that the efficiency of
heat distribution from the day-side to the night-side of the planet is
extremely inefficient. Our results are consistent with the fact that such large
day-side fluxes can be obtained only if there is no rotation of the atmosphere.
Additionally, we infer light curves of the planet for a full orbit in the two
Warm Spitzer bandpassses for the two cases of rotation and discuss the
observational differences.
