HR: 15:00h
AN: SH42D-06    [PDF]
TI: Comparison of Observed Coronal EUV and X-Ray Emission with that from Heating Models
AU: * Lionello, R
EM: Roberto.Lionello@saic.com
AF: Science Applications International Corporation, 10260 Campus Point Dr., San Diego, CA 92121-1578 United States
AU: Mok, Y
EM: ymok@uci.edu
AF: University of California, Irvine, Department of Physics and Astronomy, 4129 Frederick Reines Hall, Irvine, CA 92697-4575 United States
AU: Linker, J A
EM: Jon.A.Linker@saic.com
AF: Science Applications International Corporation, 10260 Campus Point Dr., San Diego, CA 92121-1578 United States
AU: Miki\'c, Z
EM: Zoran.Mikic@saic.com
AF: Science Applications International Corporation, 10260 Campus Point Dr., San Diego, CA 92121-1578 United States
AB: 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.
DE: 7509 Corona
DE: 7524 Magnetic fields
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting