34th Solar Physics Division Meeting, June 2003
Session 4 Corona II
Poster, Monday, June 16, 2003, 3:30-5:00pm, Mezzanine

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[4.03] Parametric Dependence of Coronal Heating Mechanisms and Active-Region Emissions

Y. Mok (U.C. Irvine), R. Lionello, Z. Mikic, J. Linker (SAIC, San Diego)

The thermal structure of an active region depends on the mechanism that heats the coronal plasma. A number of coronal heating mechanisms have been proposed over the years. They have different parametric dependences on the magnetic field, plasma density, and possibly other variables. Different mechanisms result in different thermal structures, and therefore, different EUV and soft X-ray emissions from an active region. Hence, the comparison between the computed emissions based on these models and the observed emissions will help to discover the parametric dependences of the actual heating mechanism and put some restrictions on the theoretical models. We have developed a 3D thermo-magnetohydrodynamic code to compute the thermal structure of an active region. The emissions resulted from various heating models will be compared with the images obtained from SOHO and Yohkoh.

This work is supported by the Sun-Earth Connection Theory Program of NASA.

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