Solar wind calculation model predicts bow-shape geometry of the termination shock

Details Solar wind calculation model predicts bow-shape geometry of the termination shock Solar wind calculation model predicts bow-shape geometry of the termination shock

May 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agusmsh23a..04w&link_type=abstract

American Geophysical Union, Fall Meeting 2007, abstract #SH23A-04

Physics

2124 Heliopause And Solar Wind Termination, 2152 Pickup Ions, 2164 Solar Wind Plasma

Scientific paper

We use the solar wind calculation model to study the long-term averaged condition of the global termination shock. Input function at 1 AU is generated from Ulysses data; the solar wind from 1 AU to the immediate upstream of the shock is calculated using the pickup proton MHD equations; and the shock conditions are calculated using the Rankine-Hugoniot relations. Previously, the model has calculated the expansion and contraction of the termination shock over the solar cycle, and Voyager's encounters with the termination shock. In this study the model predicts that the termination shock has a bow-shaped open geometry (not a closed geometry). Immediately inside the shock the wind speed and temperature are not axi-symmetrical about the x-axis pointing in the anti-apex direction, however, the Mach number and shock geometry are not far from axi-symmetry. The shock strength decreases at increasing distance from the nose of the shock and from the x-axis; eventually, the shock is reduced to a Mach wave across which there is no jump in flow parameters and flow direction. The postshock flow condition provides the boundary condition for the plasma flow in the heliosheath. In the sheath region, the flow is subsonic in a limited region near the nose and it becomes supersonic elsewhere outside a sonic line; the flow gradually turns away from x-axis first, and then also turns toward the downwind direction.

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