AAS 204th Meeting, June 2004
Session 54 Solar Flares
SPD Poster, Wednesday, June 2, 2004, 10:00am-7:00pm, Ballroom

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[54.02] RHESSI and Microwave Imaging Observations of Two Solar Flares

M. R. Kundu, E. J. Schmahl, V. I. Garaimov (University of Maryland)

We present hard X-ray (RHESSI) and microwave (NoRH) imaging observations of two solar flares of M-class observed on March 14 and March 12 of 2002, one located near the disk center and the other near the E-limb. For the March 14 event (near disk center), both hard X-ray and microwave observations indicate that the flaring region consisted of a complex of multiple loops. In microwaves its spatial configuration has a double-loop structure; at the main flare site (primary flaring loop) we observe microwave, HXR, EUV emissions and at a remote site (connected to main site by a long loop) we observe microwaves only due to a strong magnetic field. Some HXR foot point sources (in 25-100 KeV bands) have co-located microwave footpoint sources. The hard X-ray spectrum can be fitted with a thick target model with a thermal component and a broken power-law component. The March 12 E-limb event was fully observed by Nobeyama Radio Heliograph (NoRH), but in hard X-rays it was observed only from around the peak until the end of flare, because of RHESSI night time. In hard X-rays (6-50 KeV) it was clearly a coronal source located above an EIT loop, and it seems to have significant motion in the post flare period. In microwaves it was also a coronal source in both 17 and 34 GHz. Due to the relatively poor resolution of NoRH, the overall source size in radio is large, encompassing the RHESSI source at the start and end of its motion. The spatial maximum of the 17 GHz source appears at a coronal height below the HXR source. The microwave source also shows motion, along with the expansion of the EIT flaring loop. The hard-ray spectral properties of the flare will be discussed.

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