Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995adspr..16...71s&link_type=abstract
Advances in Space Research (ISSN 0273-1177), vol. 16, no. 4, p. (4)71-(4)74
Astronomy and Astrophysics
Astronomy
1
Boundary Layer Plasmas, Planetary Ionospheres, Plasma Sheaths, Solar Wind, Venus (Planet), Very Low Frequencies, Astronomical Models, Pioneer Venus 1 Spacecraft, Planetary Magnetospheres, Plasma Acceleration, Plasma Heating, Solar Planetary Interactions, Wave-Particle Interactions
Scientific paper
At Venus the interaction of the shocked solar wind and cold planetary ions takes place in the dayside mantle. The shocked solar wind is a warm, drifting Maxwellian plasma whereas the planetary plasma is cold; the plasma in the mantle is strongly magnetized. The coexistence of these two populations is unstable, and it leads to wave excitations that organize the energy and momentum exchange between the shocked solar wind and the plasma of planetary origin. The source of the free energy is the solar wind. The intensive wave activity seen in the 100 Hz channel of the wave instrument onboard the Pioneer-Venus Orbiter in the dayside mantle region of Venus can be identified as almost electrostatic VLF waves excited by the kinetic branch of the modified two-stream lower hybrid instability. The waves interact with the particles, and the planetary plasma is heated and accelerated outside the ionosphere, close to its upper boundary. This way solar wind scavenges the ionosphere, and planetary ions leave the planetary magnetosphere. A portion of the wave energy is capable of penetrating directly into the ionosphere and heating it.
Nagy Andrew F.
Ride S. K.
Shapiro Vitali D.
Shevchenko V. I.
Szegö Karoly
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