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We present the first three-dimensional magnetohydrodynamic (MHD) simulationsof the atmosphere of HD 209458b which self-consistently include reduction ofwinds due to the Lorentz force and Ohmic heating. We find overall windstructures similar to that seen in previous models of hot Jupiter atmospheres,with strong equatorial jets and meridional flows poleward near the day side andequatorward near the night side. Inclusion of magnetic fields slows those windsand leads to Ohmic dissipation. We find wind slowing ranging from 10%-40% forreasonable field strengths. We find Ohmic dissipation rates ~10^17 W at 100bar, orders of magnitude too small to explain the inflated radius of thisplanet. Faster wind speeds, not achievable in these anelastic calculations, maybe able to increase this value somewhat, but likely will not be able to closethe gap necessary to explain the inflated radius. We demonstrate that thediscrepancy between the simulations presented here and previous models is dueto inadequate treatment of magnetic field geometry and evolution. Inducedpoloidal fields become much larger than those imposed, highlighting the needfor a self-consistent MHD treatment of these hot atmospheres.

Magnetohydrodynamic Simulations of the Atmosphere of HD 209458b