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L. L. Lundquist, G. H. Fisher, J. M. McTiernan (Space Sciences Laboratory), S. Regnier (Montana State University)
We have developed a steady-state energy balance model of the solar corona, which calculates coronal magnetic field structure and thermodynamics from a photospheric magnetogram. The method involves solving an energy equation along individual coronal loops, allowing for flows, gravity, non-uniform heating, and cross-sectional area variations. The calculated emissivities are then interpolated to a 3-d grid and used to create synthetic X-ray and EUV emission images. Comparing observed coronal images from satellite data with theoretical images generated using different assumptions about the heating term can yield observational constraints on coronal heating mechanisms. This work was supported by a DoD/AFOSR MURI grant, ``Understanding Magnetic Eruptions and their Interplanetary Consequences."
The author(s) of this abstract have provided an email address for comments about the abstract: loraine@socrates.berkeley.edu
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Bulletin of the American Astronomical Society, 36 #2
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