South-polar features on Venus similar to those near the north pole

Piccioni, G.; Drossart, P.; Sánchez‐Lavega, A.; Hueso, R.; Taylor, F. W.; Wilson, Colin; Grassi, D.; Zasova, L.; Moriconi, M. L.; Adriani, A.; Lebonnois, Sébastien; Coradini, A.; Bézard, Bruno; Angrilli, Francesco; Arnold, Gabriele; Baines, K. H.; Bellucci, G.; Benkhoff, J.; Bibring, J. P.; Blanco, A.; Błęcka, M. I.; Carlson, R. W.; Lellis, A. Di; Encrenaz, T.; Erard, S.; Fonti, S.; Formisano, V.; Fouchet, Thierry; Garcia, Raphaël; Haus, Rainer; Helbert, J.; Ignatiev, N.; Irwin, Patrick; Langevin, Y.; López‐Valverde, M. A.; Luz, D.; Marinangeli, L.; Orofino, V.; Rodin, A. V.; Roos-Serote, M.; Saggin, Bortolino; Stam, Daphné; Titov, D. V.; Visconti, Guido; Zambelli, Massimo; Ammannito, E.; Barbis, Alessandra; Berlin, R.; Bettanini, C.; Boccaccini, A.; Bonnello, Guillaume; Bouyé, M.; Capaccioni, F.; Moinelo, Alejandro Cardesin; Carraro, Francesco; Cherubini, Giovanni; Cosi, M.; Dami, Michele; Nino, Maurizio De; Vento, Davide Del; Giampietro, M. Di; Donati, Alessandro; Dupuis, Olivier; Espinasse, S.; Fabbri, Anna Adele; Fave, Agnès; Veltroni, I. Ficai; Filacchione, G.; Garceran, K.; Ghomchi, Y.; Giustini, Maurizio; Gondet, B.; Hello, Y.; Henry, Florence; Höfer, Stefan; Huntzinger, G.; Kachlicki, J.; Knoll, René; Driss, Kouach; Mazzoni, Alessandro; Melchiorri, R.; Mondello, Giuseppe; Monti, Francesco; Neumann, Christian; Nuccilli, F.; Parisot, J.; Pasqui, Claudio; Perferi, Stefano; Peter, G.; Piacentino, Alain; Pompei, C.; Réess, Jean-Michel; Rivet, Jean‐Pierre; Romano, Antonio Wilson; Russ, Natalie; Santoni, Massimo; Scarpelli, Adelmo; Sémery, Alain; Soufflot, A.; Stefanovitch, Douchane; Suetta, Enrico; Tarchi, F.; Tonetti, Nazzareno; Tosi, F.; Ulmer, B.

doi:10.1038/nature06209

Cited by 110 publications

(91 citation statements)

References 15 publications

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“…Images taken through 2-µm filters from IR2 suggest that the vortex structure persists in the middle cloud layer seen on the nightside, consistent with the VIRTIS observations. Generally the equatorward edge of the vortex over the poles is seen in all of the LIR images, depicting its temporal evolution due to the vortex dynamics (Garate-Lopez et al 2013Limaye et al 2009;Piccioni et al 2007a). …”

Section: Global Organization Of the Cloud Cover: Vortex Situated Overmentioning

confidence: 99%

“…Galileo was the first spacecraft to map Venus between 0.7 and 5.2 µm from the near-infrared mapping spectrometer (NIMS) using the spacecraft spin and motion (Carlson et al 1991). The mapping channel of the visible infrared thermal imaging spectrometer (VIRTIS) also on Venus Express imaged the planet between 0.28 and 5.0 µm during April 15, 2006-November 27, 2014(Piccioni et al 2007a, and provided the widest spectral coverage of the southern polar hemisphere of Venus at low spatial resolution and limited coverage of the low southern and equatorial northern latitudes at higher spatial resolution (as high as a few hundred meters at periapsis). Both VMC and VIRTIS predominantly provided a polar view of the Venus cloud cover at ~ 25-45 km per pixel size and more detailed views of the equatorial and northern latitudes at a spatial scale of as high as 1-2 km per pixel.…”

Section: Nightside Images Of Venus In Near Infraredmentioning

confidence: 99%

See 1 more Smart Citation

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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Section: Global Organization Of the Cloud Cover: Vortex Situated Overmentioning

confidence: 99%

Section: Nightside Images Of Venus In Near Infraredmentioning

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

View full text Add to dashboard Cite

show abstract

“…This combination of changes in the temperature and cloud structures results in the modulation of thermal flux observed from orbit. Figure 32 shows the VIRTIS thermal infrared (5 μm) mosaic captured by VIRTIS/Venus Express (Piccioni et al 2007b). The brightness temperature in low latitudes is a few tenths of degrees higher than the cold collar region at 60-70°S.…”

Section: Infrared Emissionmentioning

confidence: 99%

Venus Atmospheric Thermal Structure and Radiative Balance

et al. 2018

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From the discovery that Venus has an atmosphere during the 1761 transit by M. Lomonosov to the current exploration of the planet by the Akatsuki orbiter, we continue to learn about the planet's extreme climate and weather. This chapter attempts to provide a comprehensive but by no means exhaustive review of the results of the atmospheric thermal structure and radiative balance since the earlier works published in Venus and Venus II books from recent spacecraft and Earth based investigations and summarizes the gaps in [1411][1412][1413][1414] 1986). Thus, most of the new information about the atmospheric thermal structure has come from different remote sensing (Earth based and spacecraft) techniques using occultations (solar infrared, stellar ultraviolet and orbiter radio occultations), spectroscopy and microwave, short wave and thermal infrared emissions. The results are restricted to altitudes higher than about 40 km, except for one investigation of the near surface static stability inferred by Meadows and Crisp (J. Geophys. Res. 101:4595-4622, 1996) from 1 μm observations from Earth. Little information about the lower atmospheric structure is possible below about 40 km altitude from radio occultations due to large bending angles. The gaps in our knowledge include spectral albedo variations over time, vertical variation of the bulk composition of the atmosphere (mean molecular weight), the identity, properties and abundances of absorbers of incident solar radiation in the clouds. The causes of opacity variations in the nightside cloud cover and vertical gradients in the deep atmosphere bulk composition and its impact on static stability are also in need of critical studies. The knowledge gaps and questions about Venus and its atmosphere provide the incentive for obtaining the necessary measurements to understand the planet, which can provide some clues to learn about terrestrial exoplanets.

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“…VIMS uses wavelengths beyond 4.5 μm to image the planet bathed from within by its own thermal emission, as has been done for Venus (Baines et al 2006;Drossart et al 2007;Piccioni et al 2007). In the 5 m spectral region, the primary sources of extinction are spectrally-localized molecular absorption by trace gases (e.g., phosphine, germane, ammonia) and the extinction of deep clouds comprised of large particles with radii near or larger than 5-m.…”

Section: Cassini Probing Of the Atmosphere Below Cloud Topmentioning

confidence: 99%