On the Relation of Above-the-loop and Footpoint Hard X-Ray Sources in Solar Flares

Details On the Relation of Above-the-loop and Footpoint Hard X-Ray Sources in Solar Flares On the Relation of Above-the-loop and Footpoint Hard X-Ray Sources in Solar Flares

Aug 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011apj...737...48i&link_type=abstract

The Astrophysical Journal, Volume 737, Issue 2, article id. 48 (2011).

Astronomy and Astrophysics

Astronomy

2

Sun: Flares, Sun: Particle Emission, Sun: X-Rays, Gamma Rays

Scientific paper

We report on the most prominent example of an above-the-loop hard X-ray source in the extensive solar flare database of RHESSI. The limb flare of 2003 October 22 around 20 UT resembles the famous Masuda flare, except that only one of the footpoint sources is visible with the other one occulted. However, even for this very prominent event, the above-the-loop source is only visible during one of the four hard X-ray peaks, highlighting the rare occurrence of above-the-loop sources that are equally bright as footpoint sources. The relative timing between the above-the-loop and footpoint sources shows that the coronal source peaks about 10 s before the footpoint source and decays during the time the footpoint source is most prominent. Furthermore, the derived number of non-thermal electrons within the above-the-loop source is large enough to provide the needed number of precipitating electrons to account for the footpoint emission over the duration of the hard X-ray peak. Hence, these observations support the simple scenario where bulk energization is accelerating all electrons within the above-the-loop source and precipitating electrons are emptying out of the above-the-loop source to produce the footpoint emissions.

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