Kinetic Kelvin-Helmholtz instability at a finite sized object

Details Kinetic Kelvin-Helmholtz instability at a finite sized object Kinetic Kelvin-Helmholtz instability at a finite sized object

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995jgr...10012017t&link_type=abstract

Journal of Geophysical Research (ISSN 0148-0227), vol. 100, no. A7, p. 12,017-12,023

Physics

4

Boundary Layer Plasmas, Kelvin-Helmholtz Instability, Kinetics, Two Dimensional Models, Magnetohydrodynamic Flow, Magnetopause, Solar Wind, Venus (Planet)

Scientific paper

Two-dimensional hybrid simulations with particle ions and fluid electrons are used to calculate the kinetic evolution of the self-consistent flow around a two-dimensional obstacle with zero intrinsic magnetic field. Plasma outlfow from the obstacle is used to establish a boundary layer between the incoming solar wind and the outgoing plasma. Because the self-consistent flow solution, a velocity shear is naturally set up at this interface, and since the magnetic field for these simulations is transverse to this flow, the Kelvin-Helmholtz (K-H) instability can be excited at low-velocity shear. Simulations demonstrate the existence of the instability even near the subsolar location, which normally is thought to be stable to this instability. The apparent reason for this result is the overall time dependence at the boundary layer, which gives rise to a Rayleigh-Taylor like instability which provides seed perturbations for the K-H instability. These results are directly applicable to Venus, comets, artificial plasma releases, and laser target experiments. This result has potentially important ramifications for the interpretation of observational results as well as for an estimation of the cross-field transport. The results suggest that the K-H instability may play a role in dayside processes and the Venus ionopause, and may exist within the context of more general situations, for example, the Earth's magnetopause.

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