Temperature, Density, and Magnetic Field Reconstructions of Active Region Coronae

We present simulated coronal emission pictures of some case-study solar active regions, including NOAA-designated regions 8210 and 8038. The simulated emissions are calculated from a 3-d temperature, density, and magnetic field model of the corona based on first principles. The method involves a static energy balance along individual coronal loops, with the heating term taken from a given coronal heating theory. The predicted emissions can be compared with observed X-ray and UV satellite images. By comparing the predictions of various heating theories with observations, we can determine constraints on the probable mechanisms of coronal heating. The model is also useful for a variety of other applications, such as testing of coronal magnetic field extrapolation techniques, calculations of wave propagation and shock phenomena, and testing assumptions about the spatial distribution of heating along loops. This work was supported by a DoD/AFOSR MURI grant, "Understanding Magnetic Eruptions and their Interplanetary Consequences."