Computer Science
Scientific paper
Jun 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993adspr..13..227w&link_type=abstract
Advances in Space Research (ISSN 0273-1177), vol. 13, no. 6, p. 227-236.
Computer Science
21
Heliosphere, Interplanetary Magnetic Fields, Interstellar Matter, Plasma Interactions, Solar Wind Velocity, Computerized Simulation, Magnetic Field Configurations, Maxwell Equation
Scientific paper
Global structures of the outer heliosphere are studied here using MHD simulation in the axisymmetric system. The interplanetary helical magnetic field is found to play an important role in the outer heliosphere. A collimated plasma flow channel is formed in the heliosheath along the solar rotation axis. The flow is trapped and pinched by the surrounding helical magnetic field. It flows outward along the axis so that the domain of the heliosheath is elongated along the axis. The terminal shock is contracted by about 30 percent by the effect of the helical magnetic field. The polarity of the helical magnetic field in the heliosheath change with the 11-yr solar cycle variation. When the interstellar medium flow is oblique to the solar rotation axis, a binary parallel flow structure is formed in the tail of the outer helisphere or the tail itself may split into two parts.
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