The internal structure of a self-gravitating object with a given mass and chemical composition can be obtained through the knowledge of the equation of state with standard methods.
We aim at an organic description of the long-term evolution by connecting dynamo simulation with a given structure, to its long-term expected evolution. We mostly focus on the evolution of gas giants, where the Ohmic dissipation can play a very important role in inflating their radii, as it is seen in data.
Within that, we also study the magnetic induction in the Hot Jupiters ionized atmosphere, as a result of the strong thermal winds. We are obtaining new important results which support the presence of strong magnetic fields, with possible implication for the long-term evolution mentioned above, and the radio emission. On the other hand, we perform dynamo simulations corresponding to different stages of the planetary evolution.
MESA code used for the long-term evolution coupled with dynamo fields: https://github.com/danielevigano/mesa_ohmic_hj
Supercomputational resources awarded by the Spanish Network of Supercomputers: