International Summer Institute for Modeling in Astrophysics

We present an isolated analytical model for the ohmic heating in the interior of hot jupiters, treating the wind zone as a parameterized boundary condition. Under a conserved estimation of the strength of induced field and the assumption of an isothermal-convective planet model, we conclude that the mechanism of ohmic heating may not explain the over-inflated radius of hot jupiters along. We also develop a new time dependent evolution model for hot jupiters with ohmic heating, further show that ohmic heating is important only when the planet mass is small or the planet is at late stage of evolution.