An analysis of shock wave disturbances observed at 1 AU from 1971 through 1978

Details An analysis of shock wave disturbances observed at 1 AU from 1971 through 1978 An analysis of shock wave disturbances observed at 1 AU from 1971 through 1978

Jun 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982jgr....87.4365b&link_type=abstract

Journal of Geophysical Research, vol. 87, June 1, 1982, p. 4365-4373. Research supported by the Max C. Fleischman Foundation an

Physics

97

Plasma Diagnostics, Satellite-Borne Instruments, Shock Wave Propagation, Solar Activity Effects, Solar Protons, Solar Wind Velocity, Explorer 43 Satellite, Explorer 47 Satellite, Explorer 50 Satellite, Helium Ions, Solar Corona

Scientific paper

IMP 6, 7, and 8 data from 104 shock wave disturbances were employed to document the occurrence frequency and properties of the solar wind shock which produce He ion abundance enhancements. The shocks were identified over the 1971-1978 time period and were characterized by a preshock flow with lower than usual average bulk density, a shocked gas layer 12 hr thick, and a postshocked gas layer 1.5 days thick with a high He abundance. A high-temperature peak was found to occur in the first 12 hrs after a He-enriched shock and was not seen when He-enhancement was absent. The total pressure was also three times higher with He-shocks, and speed jumps were greater than 50 km/sec in 56% of the He events. It is concluded that all shock waves in the solar wind at 1 AU originate in coronal mass ejection events, and the presence of He-enrichment is attributable to the geometry of the area that produced the event.

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