Venus: Atmospheric Motion and Structure from Mariner 10 Pictures

  title={Venus: Atmospheric Motion and Structure from Mariner 10 Pictures},
  author={Bruce C. Murray and Michael J. S. Belton and G. Edward Danielson and Merton E. Davies and Donald E. Gault and Bruce W. Hapke and B T O'leary and Robert Strom and Verner E. Suomi and Newell J. Trask},
  pages={1307 - 1315}
The Mariner 10 television camieras imaged the planet Venus in the visible and near ultraviolet for a period of 8 days at resolutions ranging from 100 meters to 130 kilometers. Tle general pattern of the atmospheric circulation in the upper tropospheric/lower stratospheric region is displayed in the pictures. Atmospheric flow is symmetrical between north and south hemispheres. The equatorial motions are zonal (east-west) at approxiimnately 100 meters per second, consistent with the previously… 

7. Dynamics, winds, circulation and turbulence in the atmosphere of venus

With the possible exception of the lowest one or two scale heights, the dominant mode of circulation of Venus' atmosphere is a rapid, zonal, retrograde motion. Global albedo variations in the

Cloud morphology and motions from Pioneer Venus images

The orbiter cloud photopolarimeter on the Pioneer Venus spacecraft obtained over 300 images of Venus in the ultraviolet during a 3-month period of extensive observations from January through March

Stereoscopic observations of winds on Venus

  • C. Sidi
  • Physics, Environmental Science
  • 1976

Images from Galileo of the Venus Cloud Deck

Images of Venus taken at 418 (violet) and 986 (NIR) nanometers show that the morphology and motions of large-scale features change with depth in the cloud deck, and the zonal flow field shows a longitudinal periodicity that may be coupled to the formation ofLarge-scale planetary waves.

Determination of Venus Winds by Ground-Based Radio Tracking of the VEGA Balloons

Rapid variations in balloon velocity were often detected within a single transmission (330 seconds); however, they may represent not only atmospheric motions but also self-induced aerodynamic motions of the balloon.

On the Reality of the Venus Winds

Orbiter Cloud Photopolarimeter Investigation

The first polarization measurements of the orbiter cloud photopolarimeter have detected a planet-wide layer of submicrometer aerosols of substantial visible optical thickness, of the order of 0.05 to

Polar clearing in the Venus clouds observed from the Pioneer Orbiter

PIONEER Venus 1 was put into a 24-h orbit around the planet on 4 December 1978. Since then, it has made remote sensing observations of the clouds and the overlying atmosphere at IR, visible and UV



Venera 8: Measurements of Temperature, Pressure and Wind Velocity on the Illuminated Side of Venus 1

Abstract Measurements of the temperature, pressure and wind speed in the atmosphere of Venus are reported. These were obtained with the interplanetary station Venera 8, which was the first entry

Clouds of Venus: Evidence for Their Nature

The results for the index of refraction eliminate the possibility that the visible clouds are composed of pure water or ice.

Venus: Mass, Gravity Field, Atmosphere, and Ionosphere as Measured by the Mariner 10 Dual-Frequency Radio System

Analysis of the Doppler tracking data near encounter yields a value for the ratio of the mass of the sun to that of Venus of 408,523.9 � 1.2, which is in good agreement with prior determinations

Hadley-Halley Circulation on Venus

Abstract In 1686 Halley proposed that a heat source moving over a layer of fluid would induce an average horizontal flow. Recent work on this problem is reviewed and related to the literature on

The scale height of the venus haze layer

  • R. Goody
  • Physics, Environmental Science
  • 1967

Television experiment for Mariner Mars 1971