Physics – Plasma Physics
Scientific paper
May 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993ppcn.conf..189m&link_type=abstract
In ESA, Fourth International Toki Conference on Plasma Physics and Controlled Nuclear Fusion p 189-193 (SEE N94-22624 05-75)
Physics
Plasma Physics
Kelvin-Helmholtz Instability, Magnetohydrodynamic Stability, Magnetosheath, Solar Wind, Boundary Layer Equations, Magnetohydrodynamic Flow, Plasma Density, Plasma Dynamics, Solar Terrestrial Interactions, Viscosity
Scientific paper
A two dimensional magnetohydrodynamic simulation of the Kelvin-Helmholtz instability at the terrestrial magnetospheric boundary was performed. The results show that finite thick velocity shear layer with super Alfvenic velocity jump at the magnetospheric boundary is unstable no matter how large the magnetosheath sonic Mach number. For all magnetosheath sonic Mach numbers, a velocity boundary layer is formed inside of the magnetospheric boundary due to tangential stress associated with the instability and a flow vortex is excited at the inner edge of the velocity boundary layer. The magnetospheric boundary is more highly nonlinearly corrugated by the instability for a smaller sonic Mach number. Tangential stress due to the instability at the boundary is mainly caused by Reynolds stress and is found to be large enough for exciting a residual plasma convection inside the terrestrial magnetosphere.
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