Towards a Thermodynamic 3D MHD Model of Coronal Jets

Abstract:

Transient collimated plasma eruptions in the corona, so-called "standard" and "blowout" coronal jets, are among the most intriguing manifestations of solar activity.

We have begun to use the PSI "thermodynamic" 3D MHD model to improve our understanding of the origin, dynamics, and plasma properties of coronal jets. Our code models the corona by taking into account thermal conduction, radiative cooling, empirical coronal heating, and the solar wind, and it is capable of using observed magnetograms as boundary condition for the magnetic field. Furthermore, the model is coupled with 3D MHD flux emergence simulations, i.e it can use boundary conditions provided by such simulations to drive a time-dependent coronal evolution. These properties enable us to simulate the energy transfer in coronal jetsin a more realistic manner.

We will present preliminary results.