Electron acceleration in solar flares

Details Electron acceleration in solar flares Electron acceleration in solar flares

Mar 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989soph..121...95d&link_type=abstract

(IAU, Colloquium on Solar and Stellar Flares, 104th, Stanford, CA, Aug. 15-19, 1988) Solar Physics (ISSN 0038-0938), vol. 121, n

Astronomy and Astrophysics

Astronomy

14

Electron Acceleration, Solar Electrons, Solar Flares, Spaceborne Astronomy, International Sun Earth Explorer 3, Power Spectra, Satellite-Borne Instruments, Solar Instruments

Scientific paper

For the period Spetember 1978 to December 1982, 55 solar flare particle events for which the instruments on board the ISEE-3 spacecraft detected electrons above 10 MeV. Combining data with those from the ULEWAT spectrometer electron spectra in the range from 0.1 to 100 MeV were obtained. The observed spectral shapes can be divided into two classes. The spectra of the one class can be fit by a single power law in rigidity over the entire observed range. The spectra of the other class deviate from a power law, instead exhibiting a steepening at low rigidities and a flattening at high rigidities. Events with power-law spectra are associated with impulsive (less than 1 hr duration) soft X-ray emission, whereas events with hardening spectra are associated with long-duration (more than 1 hr) soft X-ray emission. The characteristics of long-duration events are consistent with diffusive shock acceleration taking place high in the corona. Electron spectra of short-duration flares are well reproduced by the distribution functions derived from a model assuming simultaneous second-order Fermi acceleration and Coulomb losses operating in closed flare loops.

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