Magnetic field fluctuations in the Venus magnetosheath

Details Magnetic field fluctuations in the Venus magnetosheath Magnetic field fluctuations in the Venus magnetosheath

Aug 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983georl..10..655l&link_type=abstract

(Chapman Conference on Waves in Magnetospheric Plasmas, Kona, HI, Feb. 1983) Geophysical Research Letters (ISSN 0094-8276), vol.

Physics

27

Magnetic Variations, Magnetosheath, Planetary Magnetic Fields, Planetary Magnetospheres, Solar Wind, Venus Atmosphere, Bow Waves, Convective Flow, Pioneer Venus Spacecraft, Shock Waves, Time Response, Venus, Magnetosheath, Magnetic Fields, Models, Convection, Patterns, Shock, Solar Wind, Pioneer Venus, Streamlines, Periods, Polarization, Particles, Ionopause, Magnetopause, Turbulence, Bow Shock, Analysis, Obsrvations, Flow

Scientific paper

Using a model for the convection pattern of the shocked solar wind flow around the Venus obstacle, Pioneer Venus observations of ultra-low-frequency (≡10 - 40 s period) magnetic field fluctuations in the magnetosheath have been traced along streamlines to the region of the quasi-parallel bow shock. The periods and polarizations of the sinusoidal fluctuations are similar to those observed upstream of the quasi-parallel bow shock, where streaming superthermal particles are believed to produce MHD waves by a beam-plasma instability. The results suggest that both disturbances at the ionopause at Venus and the earth's magnetopause may be caused by convection of turbulent magnetic fields from the subsolar bow shock when the interplanetary field direction produces a quasi-parallel shock there.

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