HR: 15:45h
AN: SP14A-02    [Abstracts]
TI: Predicting Coronal Emissions with Multiple Heating Rates
AU: * Lundquist, L L
EM: loraine@ssl.berkeley.edu
AF: Space Sciences Laboratory, UC Berkeley, 7 Gauss Way, Berkeley, CA 94720-7450 United States
AU: Fisher, G H
EM: fisher@ssl.berkeley.edu
AF: Space Sciences Laboratory, UC Berkeley, 7 Gauss Way, Berkeley, CA 94720-7450 United States
AU: Leka, K D
EM: leka@cora.nwra.com
AF: Northwest Research Associates, Inc., Colorado Research Associates Division, 3380 Mitchell Ln., Boulder, CO 80301 United States
AU: Metcalf, T R
EM: metcalf@lmsal.com
AF: Lockheed Martin, Solar and Astrophysics Lab, 3251 Hanover St. Org. ADBS, Bldg. 252, Palo Alto, CA 94304 United States
AU: McTiernan, J M
EM: jimm@ssl.berkeley.edu
AF: Space Sciences Laboratory, UC Berkeley, 7 Gauss Way, Berkeley, CA 94720-7450 United States
AB: A variety of proposed coronal heating mechanisms remain prominent in the literature, with insufficient observational constraints to distinguish between them. In an attempt to add further constraints, we create predicted coronal emission maps of several active regions using simple parametrizations of differing theoretical heating mechanisms and compare the results to the observed coronal emissions. The results are interpolated to a 3-d grid, convolved with instrument response function, and integrated over line of sight to simulate satellite observation of the modeled loops. We also discuss those factors which dominate the differences in observed and predicted coronal emission.
DE: 7509 Corona
DE: 7524 Magnetic fields
SC: Solar Physics Division - AAS [SP]
MN: 2005 Joint Assembly