Multiple-Loop Structure of a Solar Flare from Microwave, EUV and X-Ray Imaging Data

Details Multiple-Loop Structure of a Solar Flare from Microwave, EUV and X-Ray Imaging Data Multiple-Loop Structure of a Solar Flare from Microwave, EUV and X-Ray Imaging Data

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002mwoc.conf..233g&link_type=abstract

Multi-Wavelength Observations of Coronal Structure and Dynamics -- Yohkoh 10th Anniversary Meeting. Proceedings of the conferenc

Computer Science

Scientific paper

We present the results of analysis of a flare event of importance M2.8 that occurred at 00:56 UT Aug 28, 1999. The analysis is based upon observations made with the Nobeyama Radio Heliograph(NoRH) and Polarimeters(NoRP), TRACE, SOHO/MDI,EIT and Yohkoh/SXT. MDI, TRACE, EIT, Soft X-ray and radio images show a very complex structure of the flaring region. Pre-flare TRACE and EIT images at 00:24UT show a small brightening in the region before the flare occurred. The active region in which the flare occurred had changing magnetic fields, and a new magnetic flux seems to have emerged. The X-Ray and radio time profiles for this event show a double peaked structure. The polarimeter data showed that the maximum radio emission (1200sfu) occurred at 9.4 GHz. At 17GHz there appears to be four different radio sources including the main spot and the main flare loop. Most of the microwave emission seems to originate from the main flare loop. Comparison of BATSE and microwave time profiles at 17 and 34GHz from the main sunspot source shows that these profiles have similar structures and they coincide with the Hard X-ray peaks. The maximum of the flare loop emission was delayed by 10 sec relative to the second maximum of the sunspot associated flare emission. Analysis of SXT images during the post-flare phase shows a complex morphology - several intersecting loops and changes in the shape of the main flare loop. Implications of the complex morphology of both radio and X-ray flaring sources will be discussed.

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