Abstract
Theoretical models of magnetic reconnection have been traditionally developed within the framework of magnetohydrodynamics (MHD). However, in low‐density astrophysical plasmas like those found in the magnetopause and the magnetotail, kinetic effects such as the Hall current are expected to play a significant role. We present results from externally driven magnetic reconnection simulations, within the framework of incompressible Hall MHD in 2 1/2 dimensions. We evaluate the relevance of the Hall current in the reconnection process by performing a set of simulations with different values of the Hall parameter. We compute the corresponding reconnection rates as a function of time and explore the spatial structure of the fields in the surroundings of the diffusion region.
Published Version
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