Venus: Atmospheric motion and structure from Mariner 10 pictures

B. C. Murray; M. J. S. Belton; G. Edward Danielson; M. E. Davies; D. Gault; B. Hapke; B. O'Leary; R.G. Strom; V. Suomi; N. Trask

doi:10.1126/science.183.4131.1307

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Venus: Atmospheric motion and structure from Mariner 10 pictures

B. C. Murray·M. J. S. Belton·G. Edward Danielson·M. E. Davies·D. Gault·B. Hapke·B. O'Leary·R.G. Strom·V. Suomi·N. Trask

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Abstract

The Mariner 10 television cameras 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. The 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 approximately 100 meters per second, consistent with the previously inferred 4-day retrograde rotation. Angular velocity increases with latitude. The subsolar region, and the region downwind from it, show evidence of large-scale convection that persists in spite of the main zonal motion. Dynamical interaction between the zonal motion and the relatively stationary region of convection is evidenced by bowlike waves.

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B. C. Murray, M. J. S. Belton, G. Edward Danielson, M. E. Davies, D. Gault, B. Hapke, B. O'Leary, R.G. Strom, V. Suomi, N. Trask. 1974. Venus: Atmospheric motion and structure from Mariner 10 pictures. https://doi.org/10.1126/science.183.4131.1307

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