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George Fisher   Submitted: 2008-05-21 14:31

In Paper I, we introduced and tested a method for predicting solar active region coronal emissions using magnetic field measurements and a chosen heating relationship. Here, we apply this forward-modeling technique to 10 active regions observed with the Mees Solar Observatory Imaging Vector Magnetograph and the Yohkoh Soft X-ray Telescope. We produce synthetic images of each region using four parameterized heating relationships depending on magnetic field strength and geometry. We find a volumetric coronal heating rate (dEH/dV , not to be confused with dEH/dA quoted by some authors) proportional to magnetic field and inversely proportional to fieldline loop-length (BL-1) best matches observed coronal emission morphologies. This parameterization is most similar to the steady-state scaling of two proposed heating mechanisms: van Ballegooijen?s "current layers" theory, taken in the AC limit, and Parker?s "critical angle" mechanism, in the case where the angle of misalignment is a twist angle. Although this parameterization best matches the observations, it does not match well enough to make a definitive statement on the nature of coronal heating. Instead, we conclude that (1) the technique requires better magnetic field measurement and extrapolation techniques than currently available, and (2) forward-modeling methods that incorporate properties of transiently heated loops are necessary to make a more conclusive statement about coronal heating mechanisms.

Authors: Lundquist L. L., Fisher G. H., Metcalf T. R., Leka K. D., McTiernan J. M.
Projects: None

Publication Status: ApJ (accepted)
Last Modified: 2008-09-23 21:01
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