Effects of the Martian Magnetic Anomalies on the Tail
When the magnetic anomalies are not on the day side they can cause large scale
changes in the tail plasma properties. In the figures below, single ion
fluid simulations were run with the magnetic anomalies rotated to different
locations. The changes are then compared to when no magnetic anomalies are
present (as viewed from the south pole). When the nightside density at the
planetary simulation boundary is 1/10th the dayside density, the plasma voids
and stagnation points in the tail are enhanced.
Streamlines of the plasma flow show that the magnetic anomalies don't
neccessarily deflect plasma flow to the surface. They can actually cause an
increase in plasma flow to the surface in the neighboring regions. All of the
streamlines are started at the same location for all 4 cases.
Still unresolved is if the plasma is of solar wind or ionospheric origin.
The temperature suggests the plasma asymmetries are of ionospheric origin but
multi-fluid simulations are needed to make unequivocal predictions.
The total magnetic field for all 4 configurations. The density of magnetic
fieldlines does not indicate magnitude. Instead lines are drawn to give a
detailed view of the magnetic field geometry.
eharnett at ess.washington.edu
Last modified: Tue Jun 22 14:23:39 PDT 2004
