Galileo Infrared Imaging Spectroscopy Measurements at Venus

  title={Galileo Infrared Imaging Spectroscopy Measurements at Venus},
  author={Robert W. Carlson and Kevin H. Baines and T. Encrenaz and Fredric W. Taylor and Pierre Drossart and Lucas W. Kamp and James B. Pollack and Emmanuel Lellouch and A. D. Collard and Simon Calcutt and David H. Grinspoon and Paul R. Weissman and William Smythe and Adriana C. Ocampo and G. Edward Danielson and Fraser P. Fanale and Torrence V. Johnson and Hugh H. Kieffer and Dennis Matson and Thomas B. McCord and Laurence A. Soderblom},
  pages={1541 - 1548}
During the 1990 Galileo Venus flyby, the Near Infaied Mapping Spectrometer investigated the night-side atmosphere of Venus in the spectral range 0.7 to 5.2 micrometers. Multispectral images at high spatial resolution indicate substanmial cloud opacity variations in the lower cloud levels, centered at 50 kilometers altitude. Zonal and meridional winds were derived for this level and are consistent with motion of the upper branch of a Hadley cell. Northern and southern hemisphere clouds appear to… 

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

Multispectral near-IR imaging of Venus nightside cloud features

Near-infrared imaging observations of the Venus nightside were made on May 17–23, 1996, at the Apache Point Observatory. The data were taken with an acousto-optic tunable filter camera (AOTF), which

Ground-Based Near-Infrared Imaging Observations of Venus During the Galileo Encounter

Maps of the water vapor distribution show no evidence for large horizontal gradients in the lower atmosphere of Venus, suggesting that they are produced at different altitudes.

Galilean Satellite Observation Plans for the Near Infrared

On December 7, 1995, the Galileo spacecraft will begin observations of the Jovian system with orbit insertion and a satellite tour of 10 orbits. The Galilean satellites will be observed with four

Earth global mosaic observations with NIMS-Galileo

Middle Infrared Thermal Maps of Venus at the Time of the Galileo Encounter

Images of the disk of Venus, obtained a few days after the Galileo spacecraft's closest approach on 8 February 1990; these images show variations in the thickness of the main H2SO4 cloud deck and the overlying temperature structure.

Detection of Sub-Micron Radiation from the Surface of Venus by Cassini/VIMS

Abstract We report the first detection and profile characterization of thermal emission from the surface of Venus at 0.85 and 0.90 μm, observed in the first planetary spectrum acquired by the

Characterization of mesoscale gravity waves in the upper and lower clouds of Venus from VEX‐VIRTIS images

[1] Images obtained from the Visible and InfraRed Thermal Imaging Spectrometer (VIRTIS)-M instrument onboard Venus Express present visible trains of alternating bands of cloud brightness in two



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.

Ground-Based Near-Infrared Imaging Observations of Venus During the Galileo Encounter

Maps of the water vapor distribution show no evidence for large horizontal gradients in the lower atmosphere of Venus, suggesting that they are produced at different altitudes.

The dark side of Venus

  • D. Allen
  • Physics, Environmental Science
  • 1987

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

Structure of Venus's atmosphere from modelling of night-side infrared spectra

The surface and lower atmosphere of Venus lie below long path-lengths of carbon dioxide and water vapour, and thick cloud layers that were, until recently, thought to be essentially opaque to

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The deep atmosphere of Venus revealed by high-resolution nightside spectra

THE night side of Venus is anomalously bright in two narrow spectral windows centred at 1.74 and 2.3 µm (ref. 1). The source of this emission has been identified recently as thermal radiation from

Zonal and meridional circulation of the lower atmosphere of Venus determined by radio interferometry

From earth-based Doppler and interferometric radio observations we determined the paths, in three dimensions and as functions of time, taken by the Pioneer probes as they fell to the surface of

Cloud motions on Venus - Global structure and organization

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