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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[2.62] Fine Structure in Solar Flares

H.P. Warren (CfA)

The high spatial resolution (0.5 arcsec) and broad temperature response (104-107\,K) of the Transition Region and Coronal Explorer (TRACE) make it a unique instrument for observing solar flares. Here we present analysis of several large two-ribbon flares observed with both TRACE and Yohkoh. The high spatial resolution TRACE observations show that solar flare plasma is generally not confined to a single loop or even a few isolated loops, but a multitude of fine coronal structures. These observations also suggest that the high temperature flare plasma generally appears diffuse while the cooler (<2\,MK) post-flare plasma is loop-like. We conjecture that the diffuse appearance of the high temperature flare emission seen with TRACE is due to a combination of the emission measure structure of these flares and the instrumental temperature response and does not reflect fundamental differences in plasma morphology at the different temperatures.

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