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Magnetically-driven hotspot variations (which are tied to atmospheric windvariations) in hot Jupiters are studied using non-linear numerical simulationsof a shallow-water magnetohydrodynamic (SWMHD) system and a linear analysis ofequatorial SWMHD waves. In hydrodynamic models, mid-to-high latitudegeostrophic circulations are known to cause a net west-to-east equatorialthermal energy transfer, which drives hotspot offsets eastward. We find that astrong toroidal magnetic field can obstruct these energy transportingcirculations. This results in winds aligning with the magnetic field andgenerates westward Lorentz force accelerations in hotspot regions, ultimatelycausing westward hotspot offsets. In the subsequent linear analysis we findthat this reversal mechanism has an equatorial wave analogy in terms of theplanetary scale equatorial magneto-Rossby waves. We compare our findings tothree-dimensional MHD simulations, both quantitively and qualitatively,identifying the link between the mechanics of magnetically-driven hotspot andwind reversals. We use the developed theory to identify physically-motivatedreversal criteria, which can be used to place constraints on the magneticfields of ultra-hot Jupiters with observed westward hotspots.

The Magnetic Mechanism for Hotspot Reversals in Hot Jupiter Atmospheres