Electron Acceleration and Transport During the November 5, 1998 Solar Flare At ˜13:34 UT

Details Electron Acceleration and Transport During the November 5, 1998 Solar Flare At ˜13:34 UT Electron Acceleration and Transport During the November 5, 1998 Solar Flare At ˜13:34 UT

Jun 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006soph..236...75t&link_type=abstract

Solar Physics, Volume 236, Issue 1, pp.75-95

Physics

2

Scientific paper

This paper deals with a detailed analysis of spectral and imaging observations of the November 5, 1998 (Hα 1B, GOES M1.5) flare obtained over a large spectral range, i.e., from hard X-rays to radiometric wavelengths. These observations allowed us to probe electron acceleration and transport over a large range of altitudes that is to say within small-scale (a few 103 km) and large-scale (a few 105 km) magnetic structures. The observations combined with potential and linear force-free magnetic field extrapolations allow us to show that: (i) Flare energy release and electron acceleration are basically driven by loop loop interactions at two independent, low lying, null points of the active region magnetic field; (ii) <300 keV hard X-ray-producing electrons are accelerated by a different process (probably DC field acceleration) than relativistic electrons that radiate the microwave emission; and (iii) although there is evidence that hard X-ray and decimetric/metric radio-emitting electrons are produced by the same accelerator, the present observations and analysis did not allow us to find a clear and direct magnetic connection between the hard X-ray emitting region and the radio-emitting sources in the middle corona.

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