Cloud Images from the Pioneer Venus Orbiter

  title={Cloud Images from the Pioneer Venus Orbiter},
  author={Larry Travis and David Lee Coffeen and Anthony D. Del Genio and James E. Hansen and Kiyoshi Kawabata and Andrew A. Lacis and W. A. Lane and Sanjay S. Limaye and William B. Rossow and Peter H. Stone},
  pages={74 - 76}
Ultraviolet images of Venus 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 it 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. 
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
Vertical structure of the atmosphere of Venus from Pioneer Venus orbiter radio occultations
Between December 1978 and February 1979 the Pioneer Venus orbiter spacecraft returned some 140 S band and X band radio occultation measurements of the Venus atmosphere. Results from 13 measurements,
The study of Venus with amateur telescopes
Near ultraviolet and infrared continuative high resolution images of Venus with amateur equipment can contribute actively to understand the dynamics of atmosphere and surface. In this paper images
Venus in Motion An Animated Video Catalog of Pioneer Venus Orbiter Cloud Photopolarimeter Images
Images of Venus acquired by the Pioneer Venus Orbiter Cloud Photopolarimeter (OCPP) during the 1982 opportunity have been utilized to create a short video summary of the data. The raw roll by roll
Venus in motion
A comprehensive set of television pictures of Venus taken by the Mariner 10 spacecraft is presented. Included is a chronological sequence of television images illustrating the development, variety,
Structure and meteorology of the middle atmosphere of Venus: Infrared remote sensing from the Pioneer Orbiter
The structure and variability of the middle atmosphere of Venus (60 to 140 km) were studied from the Pioneer Venus orbiter by using an infrared remote sensing instrument developed from those on


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
Venus: Atmospheric Motion and Structure from Mariner 10 Pictures
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, showing evidence of large-scale convection that persists in spite of the main zonal motion.
Cloud Patterns, Waves and Convection in the Venus Atmosphere
Detailed descriptions and interpretations are provided for phenomena seen in the UV markings on Venus during the Mariner 10 encounter with that planet. The phenomena include the dark horizontal Y,
Cloud structure and heating rates in the atmosphere of Venus
  • A. Lacis
  • Environmental Science, Physics
  • 1975
Abstract Ground-based observations and Venera 8 entry probe measurements are used to infer the vertical distribution of cloud particles in the atmosphere of Venus. In the cloud-top region, from a few
Interpretation of the Variation of Polarization over the Disk of Venus
Abstract The polarization of reflected sunlight is computed for model atmospheres of Venus as a function of location on the apparent planetary disk. The calculations are for both homogeneous
Interpretation of the polarization of Venus
Abstract The linear polarization of sunlight reflected by Venus is analyzed by comparing observations with extensive multiple scattering computations. The analysis establishes that Venus is veiled by
Space-time relationships in the UV markings on Venus
Abstract Specially prepared sections of pictures taken with the Mariner 10 television cameras are composited to show the time development of UV markings at various locations on Venus. A second series
Phase angle is the angle between the sun-planet and planet-spacecraft directions. The latitudes listed are celestial latitudes, that is
  • The time given is spacecraft event time in universal time
were supported by NASA grant 33-015-165 to State University of New York at Stony Brook. A
    • 32, 1133 (1975); A. A. Lacis, ibid., p.