Realistic 3D MHD modeling of the emerging magnetic flux and corona

The dynamics of subsurface, chromospheric, and coronal turbulent magnetoconvection spans a wide range spatial and temporal scales and other properties. Using 3D realistic MHD simulations, we are able to investigate the complex interactions that drive various phenomena observed on the solar surface and in the atmosphere, such as plasma eruptions, spontaneous formation of compact magnetic structures (pores), loop and funnel-like strictures in the corona, and others. We present recent simulations of emerging magnetic flux and coronal dynamics using the 3D radiative MHD code StellarBox (Wray et al., 2018). In particular, we focus on the evolution of the thermodynamic properties and energy exchange across different layers of the solar interior and atmosphere. Comparison of the simulation results with multi-wavelength observations from SDO, IRIS, and Hinode will be also discussed.