Zonal winds and the angular momentum balance of Venus' atmosphere within and above the clouds

Details Zonal winds and the angular momentum balance of Venus' atmosphere within and above the clouds Zonal winds and the angular momentum balance of Venus' atmosphere within and above the clouds

Oct 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985jats...42.1982w&link_type=abstract

Journal of the Atmospheric Sciences (ISSN 0022-4928), vol. 42, Oct. 1, 1985, p. 1982-1990. Research sponsored by Aerospace Corp.

Computer Science

22

Angular Momentum, Atmospheric Circulation, Middle Atmosphere, Venus Atmosphere, Venus Clouds, Northern Hemisphere, Pioneer Venus 1 Spacecraft, Wind Velocity, Venus, Zones, Winds, Angular Momentum, Atmosphere, Clouds, Temperature, Pressure, Radio Methods, Occultations, Pioneer Venus Orbiter, Latitude, Pvo, Features, Velocity, Comparisons, Altitude, Acceleration, Thermal Effects, Tidal Effects

Scientific paper

Temperatures and pressures inferred from radio occultation data acquired by the Pioneer Venus orbiter between September 1982 and November 1983 are used to derive cyclostrophic zonal winds in the middle atmosphere of Venus (1350 to 2.1 mb, 10 deg to 70 deg latitude). The main feature of the wind field is a jet positioned just above the cloud tops at 70 km and approximately 48 deg latitude. The maximum speed of the jet is about 130 m/s. A comparison with results of similar analyses on Pioneer Venus radio occultation data obtained between December 1978 and October 1981 suggests an equatorward shift of the jet and a decrease in jet speed during this five-year time interval. It is proposed that the poleward transport of westward zonal momentum by the upper branch of the cloud level Hadley cell supplies the excess momentum of the jet and maintains it against dissipation. The location of the jet thereby provides a minimum estimate of the latitudinal extent of the Hadley cell. Cyclostrophic zonal wind velocities decrease with height above about 70-75 km. It is suggested that this deceleration of the superrotation in equatorial latitudes is due to the dissipation of vertically propagating thermal tides forced primarily at altitudes around 65 km.

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