HR: 1330h
AN: SM23B-10    [Abstracts]
TI: The Current Sheet Structure in Incompressible Hall Magnetic Reconnection
AU: * Gomez, D O
EM: dgomez@df.uba.ar
AF: Instituto de Astronomia y Fisica del Espacio, CC 67 - Suc. 28, Buenos Aires, 1428 Argentina
AU: * Gomez, D O
EM: dgomez@df.uba.ar
AF: Department of physics, University of Buenos Aires, Av. Cantilo 2620, Buenos Aires, 1428 Argentina
AU: Morales, L F
EM: laura@astro.umontreal.ca
AF: Departement de Physique, Universite de Montreal, CP 6128 - succ. Centre-Ville, Montreal, 6128 Canada
AU: Dasso, S
EM: sdasso@iafe.uba.ar
AF: Instituto de Astronomia y Fisica del Espacio, CC 67 - Suc. 28, Buenos Aires, 1428 Argentina
AU: Dasso, S
EM: sdasso@iafe.uba.ar
AF: Department of physics, University of Buenos Aires, Av. Cantilo 2620, Buenos Aires, 1428 Argentina
AB: Theoretical models of magnetic reconnection have been traditionally developed within the framework of magnetohydrodynamics (MHD). However, for reconnection events taking place at the Earth's magnetopause and magnetotail, the importance of kinetic effects such as the Hall current has recently been acknowledged. In this work, we present results from parallel simulations of the incompressible Hall MHD equations in 2½ dimensions, and quantitatively investigate the relevance of the Hall effect 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. We also present a family of exact stationary solutions for the Hall MHD equations in 2½ dimensions. We compare the analytically derived spatial structure of the electric current density (and of other physical quantities) against the results obtained from the simulations.
DE: 2724 Magnetopause, cusp, and boundary layers
DE: 2744 Magnetotail
DE: 7835 Magnetic reconnection
DE: 7843 Numerical simulation studies
SC: SPA-Magnetospheric Physics [SM]
MN: 2005 Joint Assembly