Characteristics of solar-flare proton fluxes in the auroral oval in relation to the disturbance level of the magnetosphere

Details Characteristics of solar-flare proton fluxes in the auroral oval in relation to the disturbance level of the magnetosphere Characteristics of solar-flare proton fluxes in the auroral oval in relation to the disturbance level of the magnetosphere

Apr 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982ge%26ae..22..187m&link_type=abstract

Geomagnetizm i Aeronomiia, vol. 22, Mar.-Apr. 1982, p. 187-191. In Russian.

Physics

Auroral Zones, Magnetospheric Instability, Solar Cosmic Rays, Solar Flares, Solar Protons, Solar Terrestrial Interactions, High Energy Interactions, Interplanetary Magnetic Fields, Magnetic Storms, Proton Flux Density, Spatial Distribution

Scientific paper

Spatial distributions of proton fluxes with proton energies exceeding 5 MeV and 90 MeV in the high-latitude magnetosphere are obtained for the period 1969-1978. The constants of proton increase and decrease in the auroral oval are found to depend on local time and the magnitude of solar-cosmic-ray (SCR) anisotropy. The decrease of SCR intensity in the auroral zone is determined by the particle energy spectrum. The time variation of proton fluxes in the auroral oval from the morning and evening sides of the magnetosphere as a function of the sign of the IMF coincides with the time variation of proton fluxes in the north or south polar cap. As the geomagnetic-disturbance level increases, a displacement of the lower-latitude boundary of auroral fluxes toward lower invariant latitudes is observed.

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