Other
Scientific paper
May 2005
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsp52a..03l&link_type=abstract
American Geophysical Union, Spring Meeting 2005, abstract #SP52A-03
Other
7514 Energetic Particles (2114), 7519 Flares, 7524 Magnetic Fields, 7534 Radio Emissions, 7554 X Rays, Gamma Rays, And Neutrinos
Scientific paper
We present detailed comparisons of microwave and hard X-ray maps with H-alpha ribbons that are obtained with the Owens Valley Solar Array (OVSA), Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI), and H-alpha filtergrams at Big Bear Solar Observatory (BBSO), respectively, for the 2002 September 9 flare. Since microwave emission can be sensitive to nonthermal electrons residing in any part of the flaring volume depending on local magnetic field and observing frequency, our investigation is motivated to see whether the OVSA's imaging spectroscopy will reveal a link between typically confined hard X-ray sources and rather extended H-alpha kernels. For this event, we observe single hard X-ray source, three kernels at H-alpha blue wing, and more than five kernels at H-alpha line center. The microwave morphology changes from a large arcade-like structure at low frequencies to single dominant footpoint source at high frequencies, and indeed indicates the overall connection between the hard X-ray source and H-alpha kernels. However, one H-alpha kernel lying in an outer weak-field region has neither hard X-ray nor microwave counterparts, and the energetic particle transport to this kernel is yet to be explained by other means. Another non-standard feature of this event is that the H-alpha kernels remained fixed in space rather than separating away from the magnetic neutral line while the flare energy release was going on. We still argue, based on the multifrequency lightcurves, that all these separate components are energetically related, and the wavelength dependent morphology is perhaps due to energy threshold associated with each radiation.
Gary Dale E.
Lee Julian
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