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Comparative Planetology of Magnetic Effects in Ultrahot Jupiters

Presentation #627.02 in the session Planetary Atmospheres - Theory.

Published onApr 03, 2024
Comparative Planetology of Magnetic Effects in Ultrahot Jupiters

Planetary magnetic fields are common in our solar system, but have yet to be definitively detected in exoplanets. Ultrahot Jupiters (UHJs), the hottest class of exoplanets, are ideal candidates for exploring how magnetism can shape atmospheric structure due to the strongly irradiated dayside, which can cause thermal ionization of atmospheric species. These ions will then interact with the planet’s magnetic field as they are carried around the planet via strong winds. Using a state-of-the-art kinematic MHD approach in a 3D atmospheric model (RM-GCM), we study three different ultrahot Jupiters to test the robustness of our previous predictions for the UHJ WASP-76b and determine whether they extend to the overall UHJ population. Additionally, we post-process these models to generate high resolution emission and transmission spectra to study the effect of drag on these observables. Here I will discuss how the presence of a magnetic field changes atmospheric circulation and predicted observational trends in net Doppler shifts which may indicate the presence of a magnetic field. Magnetic atmospheric interactions are no doubt present in many existing observations of UHJs, but few theoretical works have focused on this and this work aims to identify robust high-resolution signatures that can be used to constrain the magnetic circulation patterns of UHJs.

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