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  • 1975-1979  (6)
  • 1
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    Cloud images from the Pioneer Venus Orbiter (1979)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: Ultraviolet images of Venus obtained over a 3-month period show marked evolution of the planetary-scale features in the cloud patterns. The dark horizontal 'Y' feature recurs quasi-periodically at intervals of about 4 days, but has also been absent for periods of several weeks. Bow-shaped features observed in Pioneer Venus images are farther upstream from the subsolar point than those in Mariner 10 images
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Science; 205; July 6
    Format: text
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    NASA TECHNICAL REPORTS
  • 2
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    Microwave boundary conditions on the atmosphere and clouds of Venus (1975)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: The dielectric properties of H2O/H2SO4 mixtures are deduced from the Debye equations and, for a well-mixed atmosphere, the structure of H2O and H2O/H2SO4 clouds is calculated. Various data on the planet together set an upper limit on the mixing ratio by number for H2O of about 0.001 in the lower Venus atmosphere, and for H2SO4 of about 0.00001. The polarization value of the real part of the refractive index of the clouds, the spectroscopic limits on the abundance of water vapor above the clouds, and the microwave data together set corresponding upper limits on H2O of approximately 0.0002 and on H2SO4 of approximately 0.000009. Upper limits on the surface density of total cloud constituents and of cloud liquid water are, respectively, about 0.1 g/sq cm and about 0.01 g/sq cm. The infrared opacities of 90 bars of CO2, together with the derived upper limits to the amounts of water vapor and liquid H2O/H2SO4, may be sufficient to explain the high surface temperatures through the greenhouse effect.
    Keywords: LUNAR AND PLANETARY EXPLORATION
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    NASA TECHNICAL REPORTS
  • 3
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    The clouds of Venus. II - An investigation of the influence of coagulation on the observed droplet size distribution (1977)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: An approximate numerical technique is used to investigate the influence of coagulation, sedimentation and turbulent motions on the observed droplet size distribution in the upper layers of the Venus clouds. If the cloud mass mixing ratio is less than 0.000001 at 250 K or the eddy diffusivity throughout the cloud is greater than 1,000,000 sq cm per sec, then coagulation is unimportant. In this case, the observed droplet size distribution is the initial size distribution produced by the condensation of the droplets. It is found that all cloud models with droplet formation near the cloud top (e.g., a photochemical model) must produce the observed droplet size distribution by condensation without subsequent modification by coagulation. However, neither meteoritic or surface dust can supply sufficient nucleating particles to account for the observed droplet number density. If the cloud droplets are formed near the cloud bottom, the observed droplet size distribution can be produced solely by the interaction of coagulation and dynamics; all information about the initial size distribution is lost. If droplet formation occurs near the cloud bottom, the lower atmosphere of Venus is oxidizing rather than reducing.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Journal of the Atmospheric Sciences; 34; Feb. 197
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  • 4
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    Large-scale motion in the Venus stratosphere (1979)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: To examine a postulate that the horizontal momentum exchanges in the Venusian stratosphere are quasi-nondivergent, the properties of two-dimensional turbulence on a slowly rotating sphere in a high-resolution, one-level numerical model are investigated. It is concluded that the forcing which maintains the stratospheric flow is weak and influences the dynamics far less than the inertial effects. Consequently, the behavior resembles that of vorticity-conserving, two-dimensional flows. On a slowly rotating planet like Venus, such flows are dominated by solid-body rotation and by a planetary wave of unit zonal wavenumber - this wave corresponds to the observed Y-shaped UV feature. Although these largest scales of motion stand out, the dynamic balances of the flow are fundamentally nonlinear, in contrast to the quasi-linear Rossby wave regime on rapidly rotating planets.
    Keywords: SOLAR PHYSICS
    Type: Journal of the Atmospheric Sciences; 36; Mar. 197
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  • 5
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    Cloud microphysics - Analysis of the clouds of Earth, Venus, Mars, and Jupiter (1978)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: The probable microphysics of a cloud is deduced by a described method which requires information on cloud particle mean size, composition, number density, and atmospheric structure, but does not require any additional information. The analysis is applied to the sulfuric acid clouds of Venus, the water ice and dust clouds of Mars, and the ammonia-water and ammonia ice clouds of Jupiter. The Venus cloud layer is found to have some resemblance to smog and haze layers on earth. The water ice clouds on Mars resemble tenuous nonprecipitating cirrus clouds on earth. Precipitation, vertical distribution of gases, and vertical transport of heat in the clouds on Jupiter are considered.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Icarus; 36; Oct. 197
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  • 6
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    Cloud Images from the Pioneer Venus Orbiter (1979)
    American Association for the Advancement of Science
    Details
    Publication Date: 1979-07-06
    Print ISSN: 0036-8075
    Electronic ISSN: 1095-9203
    Topics: Biology , Chemistry and Pharmacology , Computer Science , Medicine , Natural Sciences in General , Physics
    Published by American Association for the Advancement of Science
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