Atmospheric turbulence and magnetic field amplification in hot Jupiters

Hot Jupiters (HJs) are gas giants orbiting very close to their host stars. These planets have inflated radii that cannot be accounted for standard cooling models. Various mechanisms have been proposed, among which is Ohmic dissipation based on the dissipation of currents induced by the magnetic field stretching due to the flow motion. This work in progress focuses on the effect of atmospheric turbulence on magnetic fields and Ohmic dissipation in the upper atmosphere of HJs. Box simulations representing tiny atmospheric columns are used to evaluate where electrical currents are induced by the shear layer and the turbulence and quantify them. We perform ideal magnetohydrodynamic (MHD) simulations applicable for very Hot Jupiters. We find strong magnetic fields (up to kG locally) and currents at equilibrium, induced by enforcing the local effects of zonal jets and, at a lesser extent, turbulent perturbations. These models will be used to quantitatively assess
the radius inflation, by calculating the (high) conductivity profile.