Hard X-ray timing

Details Hard X-ray timing Hard X-ray timing

Jun 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aipc..374..300a&link_type=abstract

High energy solar physics. AIP Conference Proceedings, Volume 374, pp. 300-310 (1996).

Physics

7

Solar Electromagnetic Emission

Scientific paper

High-time resolution (64 ms) hard X-ray (HXR) data from BATSE/CGRO allow us to study the energy-dependent timing of acceleration, propagation, energy loss, and trapping of >~20 keV HXR-emitting electrons during solar flares. In many flares two different HXR flux components can be distinguished: (1) the fine structure of a HXR time profile (containing sequences of subsecond pulses) exhibits delays of ~=10-100 ms for the low-energy electrons, while (2) the unmodulated HXR time profile (a smooth lower envelope to the fine structure) shows a delay of opposite sign and much larger magnitude, of typically 1-10 s. We model the timing of various acceleration mechanisms and find that the delay of the HXR pulses is dominated by time-of-flight differences rather than by acceleration time scales, while the timing of the unmodulated HXR flux is governed by trapping and collisional time scales.

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