HR: 11:00h
AN: SH21C-03    [PDF]
TI: Coronal hard X-ray source accompanying a flare plasma ejection
AU: * Masuda, S
EM: masuda@stelab.nagoya-u.ac.jp
AF: Solar-Terrestrial Environment Laboratory, Nagoya University, Honohara 3-13, Toyokawa, 442-8507 Japan
AB: In many of flares occurring near the solar limb, a hot-plasma ejection is observed in soft X-rays during the impulsive phase. This is a piece of evidence to support flare models which are based on the cusp-type magnetic reconnection in the corona. Sometimes a compact hard X-ray source is observed above the soft X-ray flaring loop at the same time. This clearly indicates that the flare-energy release, probably magnetic reconnection, occurs above the soft X-ray loop. Fast reconnection downward flow impinges on the closed magnetic loops and high-energy electrons are produced there. In this scenario, the above-the-looptop hard X-ray source is closely related to the reconnection downward flow. How is the reconnection upward flow observed? Recently it is found in the impulsive phase of an M-class flare that a hard X-ray (above 20 keV) source exists slightly below a soft X-ray ejected feature which is located far above the soft X-ray flaring loop. This hard X-ray source might be a counterpart of the hard X-ray source mentioned above. This is caused by interaction between the reconnection upward flow and the hot-plasma ejection. We discuss how such high-energy electrons are produced there.
DE: 7509 Corona
DE: 7514 Energetic particles (2114)
DE: 7519 Flares
DE: 7554 X rays, gamma rays, and neutrinos
DE: 7835 Magnetic reconnection
SC: SPA - Solar and Heliospheric Physics [SH]
MN: 2003 Fall Meeting