Termination shock - Solar cycle variations of location and speed

Details Termination shock - Solar cycle variations of location and speed Termination shock - Solar cycle variations of location and speed

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993jgr....9815221w&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 98, no. A9, p. 15,221-15,230.

Physics

47

Magnetohydrodynamic Flow, Periodic Variations, Shock Waves, Solar Cycles, Solar Wind, Interstellar Matter, Mathematical Models, Rankine-Hugoniot Relation, Stagnation Pressure

Scientific paper

Plasma and magnetic field data from Voyagers 1 and 2 over an 11-year period (1978-1988) together with a one-fluid MHD model are used to study the motion of the termination shock. The observed large fluctuations in solar wind parameters cause variations in the speed, in the jump conditions, and in the location of the termination shock. If the interstellar stagnation pressure is equivalent to a magnetic field of 0.5 nT plus draping enhancements, the termination shock moves between 88 AU and 102 AU. The location of the termination shock is anticorrelated with the sunspot number. The termination shock is very strong with pressure ratios of a few thousands, the fast Mach number is about 12, and the plasma beta ratio jumps from about 0.1 to about 14. During the declining phase of the solar cycle, the shock speed is often greater than or comparable to the spacecraft speed. If the crossing of the termination shock by a spacecraft occurs during the declining phase, the spacecraft will cross the termination shock 3 or more times over a period of about 4 years.

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