HEATING OF THE SOLAR CORONA: MODELING THE EUV/X-RAY EMISSION

摘要

We use potential field extrapolations of Kitt Peak high resolution magnetograms to compute the coronal field lines of a large bright point observed on 1997, September 12. We then populate the field lines with solutions to the hydrostatic loop equations based on a form of the volumetric heating function that has been found to be consistent with observations of large active regions in previous work. We then use the computed densities and temperatures to calculate average intensities and simulated images for Yohkoh/SXT, SOHO/EIT and SOHO/CDS. The results are compared to observations and it is found that the models work well for the SXT emission and are also able to reproduce the average intensities of reliable lines over a wide range of temperatures to within ～ 50-80%. The morphology in the visualizations of the EUV emission, however, show significant differences with the observations suggesting that dynamic processes play a role in the heating. The results are also applied to modeling of the quiet Corona where similar results are found.