Venus: Atmospheric Motion and Structure from Mariner 10 Pictures

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

doi:10.1126/science.183.4131.1307

Cited by 104 publications

(33 citation statements)

References 13 publications

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“…This seems to agree with the finding of Murray et al (1974) that features 50-100 km across had lifetimes between 15 minutes (900 sec) and two hours (7200 sec); at 100 m/sec, 100 km is traversed in 1000 sec. On the other hand, if the light and dark regions were "frozen in", random motions on the order of 100 m/sec would be required -21-to make such features change; and this turbulence should quickly obliterate all UV contrast.…”

Section: Other Evidence Against High Windssupporting

confidence: 81%

Is the four-day “rotation” of venus illusory?

Young

1975

Icarus

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An overlooked systematic error exists in the apparent radial velocities of solar lines reflected from regions of Venus near the terminator, owing to a combination of the finite angular size of the Sun and its large ( 2 km/sec) equatorial velocity of rotation. This error produces an apparent, but fictitious, retrograde component of planetary rotation, typically on the order of 40 meters/sec. Spectroscopic, photometric, and radiometric evidence against a 4-day atmospheric rotation is also reviewed. The bulk of the somewhat contradictory evidence seems to favor slow motions, on the order of 5 m/sec, in the atmosphere of Venus; the 4-day "rotation" may be due to a traveling wave-like disturbance, not bulk motions, driven by the UV albedo differences.

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Section: Other Evidence Against High Windssupporting

confidence: 81%

Is the four-day “rotation” of venus illusory?

Young

1975

Icarus

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“…Later the Galileo orbiter took 77 images of Venus in reflected light from the solidstate imaging (SSI) camera (Belton et al 1991) during its Venus gravity-assisted flyby over a very short period (2.5 days) in February 1990 at two different wavelengths in reflected light (418 and 986 nm effective wavelengths). The SSI images at 418 nm showed morphologies to be similar to the Mariner 10 (Murray et al 1974) and Pioneer Venus observations (Rossow et al 1980); however, at 986 nm some differences in morphology were seen (north-south linear patterns straddling the equator). The Venus Monitoring Camera (VMC, Markiewicz 2007) on the Venus Express Orbiter (Svedhem et al 2007) imaged Venus at 365, 513, 950 and 1010 nm, and the cloud morphology has been presented by Titov et al (2008Titov et al ( , 2012.…”

Section: Dayside Images Of Venusmentioning

confidence: 97%

“…Images at 365 nm were obtained from Mariner 10, the Pioneer Venus Orbiter, and Venus Express prior to Akatsuki. The first spacecraft images were obtained over an eight-day period during the Mariner 10 flyby of Venus in February 1974 (Murray et al 1974). The morphology of the cloud cover from these images and their relationship to the Y features seen prominently in Earthbased images has been presented by Dollfus (1975).…”

Section: Dayside Images Of Venusmentioning

confidence: 99%

Venus looks different from day to night across wavelengths: morphology from Akatsuki multispectral images

Limaye

Watanabe

Yamazaki

et al. 2018

Earth Planets Space

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Since insertion into orbit on December 7, 2015, the Akatsuki orbiter has returned global images of Venus from its four imaging cameras at eleven discrete wavelengths from ultraviolet (283 and 365 nm) and near infrared (0.9-2.3 µm), to the thermal infrared (8-12 µm) from a near-equatorial orbit. The Venus Express and Pioneer Venus Orbiter missions have also monitored the planet for long periods but from polar or near-polar orbits. The wavelength coverage and views of the planet also differ for all three missions. In reflected light, the images reveal features seen near the cloud tops (~ 70 km altitude), whereas in the near-infrared images of the nightside, features seen are at mid-to lower cloud levels (~ 48-60 km altitude). The dayside cloud cover imaged at the ultraviolet wavelengths shows morphologies similar to what was observed from Mariner 10, Pioneer Venus, Galileo, Venus Express and MESSENGER. The daytime images at 0.9 and 2.02 µm also reveal some interesting features which bear similarity to the ultraviolet images. The nighttime images at 1.74, 2.26 and 2.32 µm and at 8-12 µm reveal features not seen before and show new details of the nightside including narrow wavy ribbons, curved string-like features, long-scale waves, long dark streaks, isolated bright spots, sharp boundaries and even mesoscale vortices. Some features previously seen such as circum-equatorial belts (CEBs) and occasional areal brightenings at ultraviolet (seen in Venus Express observations) of the cloud cover at ultraviolet wavelengths have not been observed thus far. Evidence for the hemispheric vortex organization of the global circulation can be seen at all wavelengths on the day-and nightsides. Akatsuki images reveal new and puzzling morphology of the complex nightside cloud cover. The cloud morphologies provide some clues to the processes occurring in the atmosphere and are thus, a key diagnostic tool when quantitative dynamical analysis is not feasible due to insufficient information.

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“…Planetary-scale waves such as the famous horizontal Y structure or the circumequatorial belts are observed in ultraviolet images (Murray, 1974;Belton et al, 1976;Anderson et al, 1978;Rossow et al, 1980;Markiewicz et al, 2007), while infrared brightness temperatures revealed wave structures like the rotating polar dipole and the wavenumber one cold collar (Taylor, 1980;Piccioni, 2007). Waves were also detected in the venusian thermosphere above 100 km by the mass spectrometer on PVO (Niemann et al, 1980;Kasprzak et al, 1988).…”

Section: Introductionmentioning

confidence: 92%