Add to ORKGImages of Venus taken at 418 (violet) and 986 [near-infrared (NIR)] nanometers show that the morphology and motions of large-scale features change with depth in the cloud deck. Poleward meridional velocities, seen in both spectral regions, are much reduced in the NIR. In the south polar region the markings in the two wavelength bands are strongly anticorrelated. The images follow the changing state of the upper cloud layer downwind of the subsolar point, and the zonal flow field shows a longitudinal periodicity that may be coupled to the formation of large-scale planetary waves. No optical lightning was detected
The Mariner 10 television cameras imaged the planet Venus in the visible and near ultraviolet for a ...
Venus has no seasons, slow rotation and a very massive atmosphere, which is mainly carbon dioxide wi...
During the 1990 Galileo Venus flyby, the Near Infaied Mapping Spectrometer investigated the night-si...
Images of Venus taken at 418 (violet) and 986 [near-infrared (NIR)] nanometers show that the morpho...
Images of Venus taken in spectral bands centered at 418 (violet) and 986 (NIR) nanometers show that ...
Near-infrared images of the Venus night side show bright contrast features that move from east to we...
At the cloud top level of Venus (65-70 km altitude) the atmosphere rotates 60 times faster than the ...
Three images of Venus have been returned so far by the Galileo spacecraft following an encounter wit...
International audienceInitial images of Venus's south pole by the Venus Express mission have shown t...
Venus is completely covered by a thick cloud layer, of which the upper part is composed of sulphuric...
For more than 8 years the Venus Monitoring Camera (VMC) onboard the Venus Express orbiter performed ...
Initial images of Venus's south pole by the Venus Express mission have shown the presence of a brigh...
Characterizing the wind speeds of Venus and their variability at multiple vertical levels is essenti...
Venus has no seasons, slow rotation and a very massive atmosphere, which is mainly carbon dioxide wi...
Venus has no seasons, slow rotation and a very massive atmosphere, which is mainly carbon dioxide wi...
The Mariner 10 television cameras imaged the planet Venus in the visible and near ultraviolet for a ...
Venus has no seasons, slow rotation and a very massive atmosphere, which is mainly carbon dioxide wi...
During the 1990 Galileo Venus flyby, the Near Infaied Mapping Spectrometer investigated the night-si...
Images of Venus taken at 418 (violet) and 986 [near-infrared (NIR)] nanometers show that the morpho...
Images of Venus taken in spectral bands centered at 418 (violet) and 986 (NIR) nanometers show that ...
Near-infrared images of the Venus night side show bright contrast features that move from east to we...
At the cloud top level of Venus (65-70 km altitude) the atmosphere rotates 60 times faster than the ...
Three images of Venus have been returned so far by the Galileo spacecraft following an encounter wit...
International audienceInitial images of Venus's south pole by the Venus Express mission have shown t...
Venus is completely covered by a thick cloud layer, of which the upper part is composed of sulphuric...
For more than 8 years the Venus Monitoring Camera (VMC) onboard the Venus Express orbiter performed ...
Initial images of Venus's south pole by the Venus Express mission have shown the presence of a brigh...
Characterizing the wind speeds of Venus and their variability at multiple vertical levels is essenti...
Venus has no seasons, slow rotation and a very massive atmosphere, which is mainly carbon dioxide wi...
Venus has no seasons, slow rotation and a very massive atmosphere, which is mainly carbon dioxide wi...
The Mariner 10 television cameras imaged the planet Venus in the visible and near ultraviolet for a ...
Venus has no seasons, slow rotation and a very massive atmosphere, which is mainly carbon dioxide wi...
During the 1990 Galileo Venus flyby, the Near Infaied Mapping Spectrometer investigated the night-si...