Other
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sm31a07e&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #SM31A-07
Other
2724 Magnetopause, Cusp, And Boundary Layers, 2740 Magnetospheric Configuration And Dynamics, 2753 Numerical Modeling, 7835 Magnetic Reconnection
Scientific paper
We present a new scenario for steady magnetic reconnection in which the point of reconnection is not a stagnation point nor can it be made a stagnation point by changing reference frames. Since the reconnection point is not a stagnation point, we name the scenario ``flow-through reconnection," FTR. FTR reveals itself in global magnetospheric MHD simulations. For the northward IMF case covered in this talk, FTR occurs on the magnetopause tailward of the dayside cusp at a magnetic null point that tips the well-known magnetic horns that MHD simulations show arise for northward IMF [Wu, 1983]. This talk will illustrate the phenomenon and show the electrodynamic situation that allows FTR to occur. The basic new point is this. The magnetic horn is a system response to the condition that the reconnection point cannot be a stagnation point for northward IMF. The system responds to this predicament by creating a long, narrow tongue (the horn) of exceptionally weak field within which the dissipation electric field exceeds the motional electric field. This situation allows the plasma to flow tailward through the reconnection point (at more than 200 km/s) while the magnetic field flows (as measured by the Poynting vector) sunward on one side of the reconnection point and tailward on the other. Wu. C. C., Shape of the magnetosphere, Geophys. Res. Lett., 10, 545, 1983.
Erickson Gary M.
Maynard Nelson C.
Schoendorf Jacqueline A.
Siebert Keith D.
Siscoe George L.
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