3D Radiative MHD Modeling of Thermodynamical Coupling from Subsurface Layers of the Sun to Corona

The dynamics of subsurface, chromospheric, and coronal turbulent magnetoconvection spans a wide range of spatial and temporal scales and other properties. Turbulent magnetoconvection is a primary driver of the dynamics and structure of the solar atmosphere and corona. Realistic high-resolution radiative MHD simulations reveal a complex multiscale structuring and dynamics above the photosphere. We present a detailed study of dynamical links between small-scale magnetic fields generated by local dynamo action and properties of the chromosphere and corona, as well as the effects of coherent self-organized magnetic structures. In particular, we discuss the formation of funnel-like strictures in the corona, eruptive dynamics, and contributions of multiscale structuring and highly non-linear dynamics to the heating of the chromosphere, transition layer, and corona. The simulations are performed using the 3D radiative MHD code StellarBox. Comparison of synthetic spectroscopic observables obtained from numerical simulations and actual observations allows us to uncover physical processes associated with observed phenomena.