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We present a detailed three-dimensional radiative-hydrodynamical simulationof the well known irradiated exoplanet HD189733b. Our model solves the fullycompressible Navier-Stokes equations coupled to wavelength-dependent radiativetransfer throughout the entire planetary envelope. We provide detailedcomparisons between the extensive observations of this system and predictionscalculated directly from the numerical models. The atmospheric dynamics ischaracterized by supersonic winds that fairly efficiently advect energy fromthe dayside to the nightside. Super-rotating equatorial jets form for a widerange of pressures from 10^-5 to 10 bars while counter rotating jets form athigher latitudes. Calculated transit spectrum agree well with the data from theinfrared to the UV including the strong Rayleigh scattering seen at shortwavelength, though we slightly under-predict the observations at wavelengthsshorter then ~0.6 microns. Our predicted emission spectrum agrees remarkablywell at 5.8 and 8 microns, but slightly over-predicts the emission at 3.6 and4.5 microns when compared to the latest analysis by Knutson et. al (2012). Oursimulated IRAC phasecurves agree fairly well with the amplitudes of variations,shape, and phases of minimum and maximum flux. However, we over-predict thepeak amplitude at 3.6 and 4.5 microns, and slightly under-predict the locationof the phasecurve maximum and minimum. These simulations include, for the firsttime in a multi-dimensional simulation, a strong Rayleigh scattering componentto the absorption opacity, necessary to explain observations in the optical andUV. The agreement between our models and observations suggest that includingthe effects of condensates in simulations as the dominant form of opacity willbe very important in future models.

Three Dimensional Radiative Hydrodynamical Simulations of the Highly Irradiated Short Period Exoplanet HD189733b