Fast electron scale magnetic reconnection in the geomagnetic tail and ionosphere

Abstract:

Fast magnetic reconnection in the geomagnetic tail in the ionosphere involves electron scale dynamics that includes the electron inertial length and finite charge separation governed by the Poisson equation. We use new forms of the partial differential equations for the electric and magnetic field during the fast reconnection dynamics that includes the whistler wave rather than the Alfven wave in wave dynamics. The ions dynamics is too slow to participate in the dynamics. The reconnections produce fast conversion of magnetic energy to supra thermal electron energy and whistler waves. The geotail reconnection events reported in by CLUSTER data may contain this type of reconnection as well as possibly in the upper ionosphere. The new formula extend to smaller scales than thos previous simulations of Horton et al. [2007] for the Nakamura et al CLUSTER data which showed electron dynamics and heating. We carry out 3D solutions of systems of partial differential equations with the electron-wave dynamics. This small scale magnetic reconnection is faster and heats the electrons directly while producing large magnetic field fluctuations. The new reconnection model may produce better agreement with the CLUSTER reconnection data [ Nakamura et al. 2006]. The small scale reconnection events are much faster than the those reported in the 2007 work. earlier. There are no particular symmetries in the fast- small scale reconnection events. The events may appear in subsections of large, irregular current sheets.