Comparing Solar Hard X-ray Emissions and Impulsive Electron Events seen at 1AU

Details Comparing Solar Hard X-ray Emissions and Impulsive Electron Events seen at 1AU Comparing Solar Hard X-ray Emissions and Impulsive Electron Events seen at 1AU

May 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusmsh22a..02k&link_type=abstract

American Geophysical Union, Spring Meeting 2004, abstract #SH22A-02

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7514 Energetic Particles (2114), 7519 Flares, 7554 X Rays, Gamma Rays, And Neutrinos

Scientific paper

The Sun frequently accelerates electrons in solar flares and type III radio bursts. Some of the accelerated electrons lose their energy by collisions in the denser, lower solar atmosphere producing hard X-ray (HXR) emissions, while others escape into interplanetary space. Whether the HXR producing and the escaping electrons are accelerated by the same mechanism is not known. We present a combined study of RHESSI X-ray observations and WIND/3dp in situ electron observations taken near 1~AU. Electron events with a solar release time in close temporal agreement with the HXR peak time are selected. For these events, the electron spectrum measured at 1~AU is compared with the electron spectrum derived from the HXR observations. We find the derived and the observed electron spectrum do not agree with a simple model of electron acceleration high in the corona with downward moving electrons producing HXRs in the lower, denser corona (thick target model) and upwards moving electrons escaping into interplanetary space without energy changes; the observed electron spectrum at 1 AU would predict a much harder HXR spectrum than what is observed. More complicated models including the effects of how particle escape from the acceleration cite are need. That a high coronal acceleration can be excluded makes it hard to explain how the low energy electrons, down to a few hundred eV, can escape to ~1~AU. This suggests that two different mechanisms may be accelerating electrons and that the HXR emission is not related to the electrons seen at 1~AU despite the close temporal correlation.

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