Numerical Simulation of the Lower-Hybrid Drift Instability: Consequences for the Venus Mantle

Details Numerical Simulation of the Lower-Hybrid Drift Instability: Consequences for the Venus Mantle Numerical Simulation of the Lower-Hybrid Drift Instability: Consequences for the Venus Mantle

Nov 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aps..dpp..4q31q&link_type=abstract

American Physical Society, Division of Plasma Physics Meeting, November 10-15, 1996, abstract #4Q.31

Physics

Plasma Physics

Scientific paper

The planetary ionospheres around the non-magnetic planets Mars and Venus are directly exposed to the shocked solar wind. An interaction between solar wind protons and the ionspheric oxygen takes place in a narrow turbulent region referred to as the plasma mantle. In this paper the microphysics of the dayside mantle is investigated numerically using a one-dimensional code that retains electron inertia. The nonlinear evolution of the lower hybrid waves propagating perpendicular to the magnetic field and destabilized by the modified two stream instability is investigated. Wave saturation is caused by electrostatic trapping of the proton species and the saturated amplitudes are shown to be in reasonable agreement with Pioneer-Venus observations. Oxygen ions pick-up and acceleration is found to be dominant by wave effects (not by E B motion), resulting in significant ion heating.

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