Expected spectropolarimetric observables in the lower solar atmosphere from 3D radiative MHD models

Abstract:

The presence of the magnetic field is critical to transport energy through the atmosphere. The next generation of telescopes will provide new insight into how the magnetic field gets into the chromosphere and its role in the solar energy balance. We have used Bifrost code to create 3D radiative MHD numerical models of the solar atmosphere with high spatial resolution (~4km). This code solves the full MHD equations with non-grey and non-LTE radiative transfer and thermal conduction along magnetic field lines. The models presented here include hydrogen ionization in non-equilibrium and ion-neutral interaction effects. These novel models show how the lower chromosphere, a region dominated by magneto-acoustic shocks and plasma beta greater than 1, is able to generate magnetic field in-situ. We have synthesized full-polarimetry Stokes profiles from these models for several spectral lines formed in the photosphere and the chromosphere. These profiles will reveal which observables are expected to be obtained by DKIST and IRIS, and how to interpret their observations according to the models and the associated profiles presented in this work.