Kinetic simulation of the Kelvin-Helmholtz instability at the Venus ionopause

Details Kinetic simulation of the Kelvin-Helmholtz instability at the Venus ionopause Kinetic simulation of the Kelvin-Helmholtz instability at the Venus ionopause

Nov 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991georl..18.1943t&link_type=abstract

Geophysical Research Letters (ISSN 0094-8276), vol. 18, Nov. 1991, p. 1943-1946. Research supported by DOE.

Physics

35

Ionopause, Ionospheric Ion Density, Kelvin-Helmholtz Instability, Magnetohydrodynamic Flow, Magnetohydrodynamic Stability, Venus Atmosphere, Computerized Simulation, Plasma Frequencies, Shear Layers, Two Dimensional Models, Wavelengths

Scientific paper

Two dimensional hybrid simulations with particles ions and fluid electrons are used to calculate the kinetic evolution of the Kelvin-Helmholtz instability at a boundary similar to the ionopause at the planet Venus. The magnetic field has been chosen to be essentially transverse to the plasma flow velocity, which is the most unstable case for the Kelvin-Helmholtz instability. Effects analogous to those found in MHD simulations are recovered, including a mode cascade to longer wavelengths. In addition, isolated structures on the order of the ion gyroradius are formed which can cross the boundary in either direction. These structures may be related to flux ropes commonly observed near the ionopause of Venus. The time evolution of these structures may represent transport across the boundary layers and the smearing of the shear layer may give rise to internal structure in the boundary. Similar processes occur in magnetized layers akin to the earth's magnetopause.

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