Propagation of low energy solar electrons

Details Propagation of low energy solar electrons Propagation of low energy solar electrons

Jul 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981georl...8..831a&link_type=abstract

Geophysical Research Letters, vol. 8, July 1981, p. 831-834.

Physics

16

Electron Energy, Electron Scattering, Interplanetary Magnetic Fields, Particle Motion, Solar Electrons, Adiabatic Conditions, Angular Distribution, Pitch (Inclination), Solar Wind

Scientific paper

Two events are reported in which 2-10 keV electrons of solar energy have undergone significant adiabatic mirroring and pitch angle scattering in large scale magnetic structures in the interplanetary medium within a distance of about 0.5 AU from the earth. Electrons of 3 keV, typical of the energies measured, have a speed of about one-tenth of the speed of light, so that their travel time from the sun at 0 deg pitch angle would be about 100 minutes. Their cyclotron radius is about 20 km for a pitch angle of 30 deg, and a field of magnitude of 5 nT, and the cyclotron period is about 7.1 milliseconds. The electrons are scattered by spatial variations in the interplanetary magnetic field. When the spatial variations are convected past a stationary spacecraft by a 500 km/sec solar wind, they are seen as temporal fluctuations at a frequency of about 3 Hz.

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