Physics
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufmsh42a..07m&link_type=abstract
American Geophysical Union, Fall Meeting 2006, abstract #SH42A-07
Physics
7514 Energetic Particles (2114), 7519 Flares, 7524 Magnetic Fields, 7526 Magnetic Reconnection (2723, 7835), 7554 X-Rays, Gamma Rays, And Neutrinos
Scientific paper
In Hα, so-called two-ribbon structure is observed during solar flares, especially long duration events. At that time, in the solar corona, an arcade structure (a group of loops connecting the two-ribbon) is often observed with soft X-ray and EUV imagers. These features are consistent with a standard magnetic reconnection model. In hard X-rays (> 30 keV), however, such a two-ribbon structure is not observed even in an arcade-type flare. Instead of that, usually a pair of compact footpoint sources is observed. Asai et al. (2002) analyzed one of such events. Comparing the hard X-ray intensity and magnetic field strength along the two ribbons, they concluded that the difference of source structure between Hα and hard X-rays was due to the poor dynamic range of the hard X-ray telescope (HXT) on board Yohkoh. Among more than 3,000 flares observed with Yohkoh/HXT, only one event showed a two-ribbon structure in hard X-rays. We analyzed this unique event which occurred on 14 July 2000, to obtain some hints for understanding acceleration mechanism of electrons in solar flares. Comparing the hard X-ray images taken with Yohkoh/HXT and the magnetic field data taken SOHO/MDI, we investigated the spatial relationship along each ribbon between magnetic field strength and hard X-ray intensity, which is directly related to the efficiency of acceleration and the amount of accelerated electrons. The general tendency of their distribution patterns is similar, but there is no clear one-to-one correspondence. The hard X-ray intensity distribution along each ribbon is more uniform than that expected from the distribution of magnetic filed strength through standard magnetic reconnection models. To understand this result correctly, the magnetic connectivity between the two ribbons might have to be considered.
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