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Hot Jupiters, with atmospheric temperatures T ~ 1000 K, have residual thermalionization levels sufficient for the interaction of the ions with the planetarymagnetic field to result in a sizable magnetic drag on the (neutral)atmospheric winds. We evaluate the magnitude of magnetic drag in arepresentative three-dimensional atmospheric model of the hot Jupiter HD209458b and find that it is a plausible mechanism to limit wind speeds in thisclass of atmospheres. Magnetic drag has a strong geometrical dependence, bothmeridionally and from the day to the night side (in the upper atmosphere),which could have interesting consequences for the atmospheric flow pattern. Byextension, close-in eccentric planets with transiently heated atmospheres willexperience time-variable levels of magnetic drag. A robust treatment ofmagnetic drag in circulation models for hot atmospheres may require iteratedsolutions to the magnetic induction and Saha equations as the hydrodynamicalflow is evolved.

Magnetic Drag on Hot Jupiter Atmospheric Winds