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T.E.K. Prozny, J.T. Schmelz (University of Memphis)
Central to solving the coronal heating problem is an understanding of the temperature structure and loop dynamics of coronal loops. It is thought that the great amounts of energy needed to heat the corona could be dumped into the lower solar atmosphere via these small magnetic loops that spring up and then disappear. Thus, by determining such characteristics as temperatures, abundances, and densities, and observing the time evolution of these loops, one can address the question of how the corona is heated. These are some of the goals focused on by The Coronal Diagnostic Spectrometer (CDS). We chose to analyze and compare CDS loops that are brightly visible in the Oxygen V line at 629.73 Angstroms with a peak formation temperature of Log T = 5.4. Our particular data set was from 2000 October 25 at 06:54 UT. Six pixels were chosen along the loop with corresponding background pixels inside and outside the loop structure. Emission lines were fit and background subtraction was performed for each pixel. We have also studied the loop dynamics and time evolution using imaging data from TRACE, EIT on SOHO, and SXT on Yohkoh. We want to compare the properties of this loop with other O V loops, including the one observed on 1999 June 30 at 19:28 UT, which we have already studied in detail. We hope to determine if the O V loops are a relative rarity, or perhaps a phase in the standard loop evolution, or even a different class of solar loop altogether. Solar physics research at the University of Memphis is supported by NASA grants NAG5-9783 and NAG5-12096.
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Bulletin of the American Astronomical Society, 36 #2
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