Numerical MHD Coronal Simulations: Energy Statistics and FORWARD Analysis.

We analyse a recent realistic radiative MHD simulation of the solar corona that was computed with the extended version of the MURaM code. The simulation covers the uppermost 8Mm of the solar convection zone and reaches 115Mm into the solar corona. The simulation covers 48 hours of solar time and simulates the evolution of a complex active region. The energy release in the corona is highly intermittent and we identify a total of 118 individual events including flares and a coronal mass ejection, which we analyse in further detail. From the simulation we compute an X-ray flux mimicking observations by the GOES (Geostationary Operational Environmental Satellite) satellite in the wavelength range 1-8 Å. The power law index for the GOES X-ray flux for flares of class C and above in this simulation is found to be 1.33452. We analyze the correlation between synthetic coronal emission during flares and the magnetic energy release in the corona. The latter is a quantity that cannot be directly determined in observations.The FORWARD code is a tool used for the purpose of coronal magnetometry. It can be used to compute synthetic observables from coronal models. We focus on the interpretation of the High Altitude Observatory's CoMP observations. The CoMP (COronal Multi-channel Polarimeter) instrument measures the intensity and the linear and circular polarisation of FeXIII at 1074.7nm.We discuss some important limitations of coronal emission line polarimetry when simulating an extremely active solar region, with emphasis on the influence of high velocities, temperatures and densities on the FORWARD output.