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Säm Krucker   Submitted: 2007-10-31 16:44

This letter presents X-ray observations of a partially limb-occulted solar flare taken by the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) and the X-ray telescope (XRT) onboard Hinode. Thermal emission originates from a simple loop at the western limb that rises slowly (~7 km s-1) until the flare peak time. Above 18 keV, faint non-thermal emission with a hard/flat spectrum (gamma ~ 4) and fast time variations (of the order of tens of seconds) is seen that comes from a loop slightly above (~2000 km) the thermal loop, if compared at the same time. However, the non-thermal loop agrees well in altitude with the thermal flare loop seen later, at the soft X-ray peak time. This is consistent with simple flare models where non-thermal electrons in a flare loop produce thin target hard X-ray emission in the corona as they travel to the loop footpoints. There they lose all their energy and heat chromospheric plasma that fills the loop earlier seen in non-thermal hard X-rays. This suggests that electron acceleration in solar flares occurs in the corona.

Authors: Säm Krucker, I.G. Hannah, R.P. Lin
Projects: Hinode,RHESSI

Publication Status: accepted
Last Modified: 2007-11-01 07:23
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