Flow downstream of the heliospheric terminal shock - The magnetic field on the heliopause

Details Flow downstream of the heliospheric terminal shock - The magnetic field on the heliopause Flow downstream of the heliospheric terminal shock - The magnetic field on the heliopause

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993jgr....9815169n&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 98, no. A9, p. 15,169-15,176.

Physics

36

Heliosphere, Magnetic Field Configurations, Magnetohydrodynamic Flow, Shock Waves, Solar Magnetic Field, Current Sheets, Flow Distribution, Mathematical Models, Plasma Dynamics

Scientific paper

Modeling the kinematic magnetic field in the solar wind beyond the terminal shock shows that a ridge of magnetic pressure is produced just inside the heliopause. This ridge is sufficiently large that it will cause the layer immediately inside the heliopause to thicken, pushing the heliopause outward and slightly affecting its position relative to the terminal shock. However, the ridge is far too thin to cause an important change in the distance of the terminal shock from the sun. We show that these conclusions are a simple consequence of geometrical arguments for incompressible, steady, laminar flows. Moreover, the heliopause magnetic field originates on the terminal shock near the sub-stagnation point. Consequently, the heliospheric current sheet field reversals are painted onto the inside surface of the heliopause. Alternate magnetic polarity strips will be oppositely directed relative to the interstellar magnetic field, implying that reconnection inevitably occurs on a fine some near the nose of the heliosphere. This suggests that the heliopause is a leaky, diffuse surface.

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