Coronal hard X-ray source accompanying a flare plasma ejection

Details Coronal hard X-ray source accompanying a flare plasma ejection Coronal hard X-ray source accompanying a flare plasma ejection

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufmsh21c..03m&link_type=abstract

American Geophysical Union, Fall Meeting 2003, abstract #SH21C-03

Physics

7509 Corona, 7514 Energetic Particles (2114), 7519 Flares, 7554 X Rays, Gamma Rays, And Neutrinos, 7835 Magnetic Reconnection

Scientific paper

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.

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