Solar Physics Division Meeting 2000, June 19-22
Session 2. Corona, Solar Wind, Flares, CMEs, Solar-stellar, Instrumentation, Other
Display, Chair: J. Krall, Monday-Thursday, June 19, 2000, 8:00am-6:00pm, Forum Ballroom

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[2.13] Diagnostic Constraints for Loop Dynamics Models

B.H. Schoepke, J.T. Schmelz, R.T. Scopes, J.W. Cirtain, C.R. Edwards (University of Memphis)

An accurate determination of the temperature distribution of a coronal loop is an essential first step to understanding the plasma emission measure, density, and filling factor. These quantities are important inputs in determining, for example, the energy balance and heating requirements, the stability, as well as the radiative losses and conductive cooling times. These loops are a basic and abundant type of coronal feature. Because they are inherently bright, they are a target of choice to learn more about the coronal structure in general. Despite much progress in recent years, the physical properties of loops are not fully understood. In fact, seemingly contradictory observations from different instruments have created conflicting ideas about their true physical properties. We have used high-resolution EUV spectral line data from SOHO-CDS and imaging data gathered simultaneously with Yohkoh-SXT to determine the temperature height structure of selected quiescent active region loops. Combining these simultaneous plasma measurements in different wavebands using different observing techniques will lead to an improved understanding of the properties and structures of coronal loops as well as provide an effective temperature cross-calibration of these two instruments. This work is supported by NASA grant NAG5-7197.

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