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Ultra-hot Jupiters represent an exciting avenue for testing extreme physicsand observing atmospheric circulation regimes not found in our solar system.Their high temperatures result in thermally ionized particles embedded inatmospheric winds interacting with the planet's interior magnetic field bygenerating current and experiencing bulk Lorentz force drag. Previoustreatments of magnetic drag in 3D General Circulation Models (GCMs) ofultra-hot Jupiters have mostly been uniform drag timescales applied evenlythroughout the planet, which neglects the strong spatial dependence of thesemagnetic effects. In this work, we apply our locally calculated active magneticdrag treatment in a GCM of the planet WASP-76b. We find the effects of thistreatment to be most pronounced in the planet's upper atmosphere, where strongdifferences between the day and night side circulation are present. Thesecirculation effects alter the resulting phase curves by reducing the hotspotoffset and increasing the day-night flux contrast. We compare our models toSpitzer phase curves which imply a magnetic field of at least 3 G for theplanet. We additionally contrast our results to uniform drag timescale models.This work highlights the need for more careful treatment of magnetic effects inatmospheric models of hot gas giants.

Exploring the Effects of Active Magnetic Drag in a GCM of the Ultra-Hot Jupiter WASP-76b