Protons with energies greater than 30 keV in the earth's radiation belts in a magnetically quiet period near the geomagnetic equator and at low altitudes

Details Protons with energies greater than 30 keV in the earth's radiation belts in a magnetically quiet period near the geomagnetic equator and at low altitudes Protons with energies greater than 30 keV in the earth's radiation belts in a magnetically quiet period near the geomagnetic equator and at low altitudes

Jan 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984kosis..22...53v&link_type=abstract

Kosmicheskie Issledovaniia (ISSN 0023-4206), vol. 22, Jan.-Feb. 1984, p. 53-66. In Russian.

Computer Science

Sound

Energy Spectra, Magnetic Equator, Proton Belts, Radiation Belts, Satellite Sounding, E Region, Energetic Particles, Proton Energy, Soviet Spacecraft

Scientific paper

The paper reports results of measurements of the differential energy spectra of protons in the 30 keV to 50 MeV energy range in the radiation belts near the geomagnetic equator, at midlatitudes, and at low altitudes (about 500 km) in magnetically quiet periods; Molniya 1 and 2, and Cosmos-900 data are examined. It is shown that these spectra are characterized by the presence of a maximum in the E-region of several hundred keV, which shifts to higher energies as L decreases. As protons are transported deep into the magnetosphere the rigidity of the high-energy tail behind the spectral maximum at L greater than 4 changes insignificantly and the pitch angle distribution is close to isotropic, in contrast to the case when L is less than 4. The region of proton precipitation is formed at L greater than 3 with a maximum at L = 6-7 in the night sector; the location of the maximum depends only slightly on L as the energy varies from 50 keV to 1 MeV. It is shown that proton spectra at low altitudes are formed under the effect of pitch angle diffusion, developing at high latitudes in the outer radiation belt.

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