Nonthermal Flare Emission from MeV - energy


We present analyses of two solar ares observed with high spatial resolution at 86 GHz with the BIMA millimeter{wavelength telescope and at 17 and 34 GHz with the Nobeyama radioheliograph. The ares were observed on Nov. 24, 1998 and May 1, 1999. At millimeter wavelengths these are impulsive events and therefore they must be produced by MeV energy electrons. The present study using simultaneous observations of two ares at 86, 34, and 17 GHz provides an excellent opportunity to study high{energy electrons with high{spatial{resolution observations at three optically{thin frequencies. The morphology of millimeter emission can reveal both the properties of the MeV{energy electrons and the nature of the coronal magnetic eld lines where they radiate. One of the two events we present is the rst clear case of a = 3 mm source in which both footpoints of a loop are detected. In the second event the polarization image at 17 GHz also suggests a bipolar or loop{like morphology. Such morphological observations can be used to constrain the nature of the magnetic eld in the solar corona.

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@inproceedings{Kundu2009NonthermalFE, title={Nonthermal Flare Emission from MeV - energy}, author={M. Rakshit Kundu and Stephen M. White and Kazuo Shibasaki and Toshimitsu Sakurai}, year={2009} }