Comparison of Observed Coronal EUV and X-Ray Emission with that from Heating Models
Abstract
The problem of finding the physical mechanism that heats the solar corona is still unsolved. Many theoretical and observational models have been proposed in the literature. In order to understand which model better reproduces the observations, we present a quantitative comparison between the emission calculated from different heating models and the observed images of an active region. This investigation uses our 3D MHD model in Cartesian coordinates, which calculates the magnetic configuration of Active Region 7986 (August, 1996) starting from a photospheric magnetogram, and another algorithm that solves the 3D fluid equations along magnetic field lines, and that includes thermal conduction, radiation losses, and the heating mechanism under investigation. Once the plasma properties are found, the emission in different wavelengths can be calculated using the Solarsoft package and can be compared with the photon counts recorded by the EIT instrument aboard the SOHO spacecraft, and the SXT instrument aboard the Yohkoh satellite.
- Publication:
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AGU Fall Meeting Abstracts
- Pub Date:
- December 2003
- Bibcode:
- 2003AGUFMSH42D..06L
- Keywords:
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- 7509 Corona;
- 7524 Magnetic fields