Evolution of recurrent solar wind structures between 14 AU and the termination shock

Details Evolution of recurrent solar wind structures between 14 AU and the termination shock Evolution of recurrent solar wind structures between 14 AU and the termination shock

Jun 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988jgr....93.5446w&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 93, June 1, 1988, p. 5446-5460.

Astronomy and Astrophysics

Astronomy

27

Interplanetary Medium, Shock Wave Propagation, Solar Wind, Astronomical Models, Magnetic Field Configurations, Magnetohydrodynamic Waves, Satellite Observation

Scientific paper

The solar wind conditions observed from Voyager 2 at approximately 14 AU are extrapolated to the region of the outer heliosphere bounded by the termination shock, using an MHD simulation model. Results from two simulation studies are presented for two sets of nearly recurrent solar wind interaction regions, with initial conditions generated from plasma and magnetic field data observed on March 1984 at 13.8 AU, and on November 1984 at 15.4, respectively. Each simulation describes an idealized recurrent solar wind structure in the supersonic region of the outer heliosphere out to the termination shock far beyond the present reaches of the Pioneer and Voyager spacecraft. It is shown that a collision between the forward shock and the reverse shock occurs approximately every 40 AU. When a forward shock interacts with the termination shock, the latter is weakened and moves outward; the termination shock is strengthened and moves inward when a reverse shock interacts with it.

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