The solar proton event of April 16, 1970. III - Evolution of pitch angle distribution as protons of not greater than 1 MeV energy propagate into the high-latitude magnetotail

Details The solar proton event of April 16, 1970. III - Evolution of pitch angle distribution as protons of not greater than 1 MeV energy propagate into the high-latitude magnetotail The solar proton event of April 16, 1970. III - Evolution of pitch angle distribution as protons of not greater than 1 MeV energy propagate into the high-latitude magnetotail

Jan 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979jgr....84..109p&link_type=abstract

Journal of Geophysical Research, vol. 84, Jan. 1, 1979, p. 109-119. NSF-supported research.

Physics

Angular Distribution, Energetic Particles, Geomagnetic Tail, Pitch (Inclination), Polar Regions, Satellite Observation, Solar Protons, Interplanetary Magnetic Fields, Ion Motion, Particle Intensity, Plasma-Particle Interactions, Vela Satellites

Scientific paper

The solar proton event of April 16, 1970 was monitored by Vela satellites in the solar wind and high-latitude magnetotail. The intensity structure at not greater than 1 MeV indicates a delay of 85-102 min in access of protons to near the center of the north lobe, corresponding to entry points at 340-370 earth radii from the earth. In three sequential periods, of 16, 181, and 124 min duration, the average intensity in the north lobe was lower, higher, and lower, respectively, than that in interplanetary space by factors that varied from 2 to 5. Pitch angle distributions were measured in three dimensions in interplanetary space and in the north lobe. The entire set of observations is consistent with an open model of the magnetotail but is not consistent with a closed model.

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