The interaction of a magnetized solar wind with the VLISM

Details The interaction of a magnetized solar wind with the VLISM The interaction of a magnetized solar wind with the VLISM

Jun 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995sowi.confq.108b&link_type=abstract

International Solar Wind 8 Conference, p. 108

Other

Heliosphere, Shock Wave Interaction, Shock Waves, Solar Wind, Interstellar Matter, Interstellar Magnetic Fields, Bow Waves, Flow Velocity, Interstellar Space

Scientific paper

The interaction of a magnetized solar wind with magnetized interstellar flow is modelled in two dimensions. The VLISM magnetic field and flow velocity are assumed to be parallel to each other and perpendicular to the sun's magnetic axis, contrast to a recent study by Washimi. The more realistic orientation of the axis and VLISM flow requires a less realistic heliospheric field model in two dimensions. The Parker spiral is replaced by a poloidal field which is tangent to the termination shock, and whose magnitude is consistent with estimates of the heliospheric field at termination shock distances. Of particular interest is the effect of the heliospheric field on the heliospheric flow beyond the termination shock, and on the structure and location of the bow shock

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