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We present a comprehensive radiative magnetohydrodynamic simulation of thequiet Sun and large solar active regions. The 197 Mm wide simulation domainspans from 18 (10) Mm beneath the photosphere to 113 Mm in the solar corona.Radiative transfer assuming local thermal equilibrium, optically-thin radiativelosses, and anisotropic conduction transport provide the necessary realism forsynthesizing observables to compare with remote sensing observations of thephotosphere and corona. This model self-consistently reproduces observedfeatures of the quiet Sun, emerging and developed active regions, and solarflares up to M class. Here, we report an overview of the first results. Thesurface magnetoconvection yields an upward Poynting flux that is dissipated inthe corona and heats the plasma to over one million K. The quiescent coronaalso presents ubiquitous propagating waves, jets, and bright points with sizesdown to 2 Mm. Magnetic flux bundles emerge into the photosphere and give riseto strong and complex active regions with over $10^{23}$ Mx magnetic flux. Thecoronal free magnetic energy, which is approximately 18\% of the total magneticenergy, accumulates to approximately $10^{33}$ erg. The coronal magnetic fieldis clearly non-force-free, as the Lorentz force needs to balance the pressureforce and viscous stress as well as drive magnetic field evolution. Theemission measure from $\log_{10}T{=}4.5$ to $\log_{10}T{>}7$ provides acomprehensive view of the active region corona, such as coronal loops ofvarious lengths and temperatures, mass circulation by evaporation andcondensation, and eruptions from jets to large-scale mass ejections.

A Comprehensive Radiative Magnetohydrodynamics Simulation of Active Region Scale Flux Emergence from the Convection Zone to the Corona