Interaction of fast steady flow with slow transient flow - A new cause of shock pair and interplanetary B(z) event

Details Interaction of fast steady flow with slow transient flow - A new cause of shock pair and interplanetary B(z) event Interaction of fast steady flow with slow transient flow - A new cause of shock pair and interplanetary B(z) event

Oct 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992jgr....9715051z&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 97, no. A10, p. 15,051-15,055.

Physics

19

Electron Flux Density, Magnetic Compression, Proton Flux Density, Solar Wind, Stellar Mass Ejection, Sun, Flux Density, Helium, Mach Number, Ratios, Steady Flow, Unsteady Flow, Velocity

Scientific paper

The occurrence of the nonspiral magnetic field (high helium density) Cold Magnetic Enhancement and counterstreaming suprathermal electron flux in the slow flow around the forward shock indicates that the slow flow is a CME in interplanetary space (ICME). The characteristics of the field and plasma in the fast flow around the reverse shock is typical for a high speed stream. Thus the shock pair here appears to be caused by the interaction of a high speed stream with a slow ICME. The fact that a -B(z) event occurred in such a shock pair suggests that the slow ICME is disconnected from the sun. It is shown that compression alone appears to be adequate to explain the large southward IMF component within the shocked plasma because of the large southward field component present in the ICME ahead of the forward shock. In addition, a new method to infer the shock angle and Mach number from the observed upstream plasma B and the jump ratios of proton density and total magnetic flux density across a shock is described.

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