Scientific goals for the observation of Venus by VIRTIS on ESA/Venus express mission

Drossart, P.; Piccioni, G.; Adriani, A.; Angrilli, Francesco; Arnold, Gabriele; Baines, K. H.; Bellucci, G.; Benkhoff, J.; Bézard, Bruno; Bibring, J. P.; Blanco, A.; Błęcka, M. I.; Carlson, R. W.; Coradini, A.; Lellis, A. Di; Encrenaz, Th.; Erard, S.; Fonti, S.; Formisano, V.; Fouchet, Thierry; Garcia, Raphaël; Haus, Rainer; Helbert, J.; Ignatiev, N.; Irwin, Patrick; Langevin, Y.; Lebonnois, Sébastien; López‐Valverde, M. A.; Luz, D.; Marinangeli, L.; Orofino, V.; Rodin, A. V.; Roos-Serote, M.; Saggin, Bortolino; Sánchez‐Lavega, A.; Stam, Daphné; Taylor, F. W.; Titov, D. V.; Visconti, Guido; Zambelli, Massimo; Hueso, R.; Tsang, C. C. C.; Wilson, Colin; Afanasenko, T. Z.

doi:10.1016/j.pss.2007.01.003

Cited by 151 publications

(102 citation statements)

References 89 publications

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“…The Akatsuki orbiter is providing equatorial, global images of Venus from its four cameras with spatial resolution comparable to or better than those obtained from the Venus Monitoring Camera (Markiewicz 2007) on Venus Express. The VIRTIS instrument on Venus Express imaged Venus in both reflected and emitted radiation between 0.28 and 5 µm (Drossart 2007;Piccioni et al 2007b) and mostly covered portions of the southern hemisphere. The Akatsuki images provide excellent symmetric views of Venus about its equator on day-and nightsides with good image quality spatial resolution from the 1024 × 1024 pixel detectors of the UVI, IR1 and IR2 cameras.…”

Section: Akatsuki Observationsmentioning

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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Section: Akatsuki Observationsmentioning

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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“…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%

Saturn Atmospheric Structure and Dynamics

Genio

Achterberg

Baines

et al. 2009

Saturn From Cassini-Huygens

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“…Following our studies of the O 2 nightglow emission (Drossart et al 2007a;Gérard et al 2008), we used the Visible and Infra-Red Thermal Imaging Spectrometer (VIRTIS) instrument Drossart et al 2007b) on the Venus Express spacecraft to look for fainter emissions on the night side of Venus. VIRTIS measures radiation intensity at wavelengths between 0.3 and 5 µm with a spectral sampling of about 10 nm in the IR.…”

Section: Observationsmentioning

confidence: 99%

First detection of hydroxyl in the atmosphere of Venus

Piccioni¹,

Drossart

Zasova

et al. 2008

A&A

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Context. Airglow emissions, such as previously observed from NO and O 2 (a− X) (0−0) on Venus, provide insight into the chemical and dynamical processes that control the composition and energy balance in the upper atmospheres of planets. The OH airglow emission has been observed previously only in the Earth's atmosphere where it has been used to infer atomic oxygen abundances. The O 2 (a − X) (0−1) airglow emission also has only been observed in the Earth's atmosphere, and neither laboratory nor theoretical studies have reached a consensus on its transition probability. Aims. We report measurements of night-side airglow emission in the atmosphere of Venus in the OH (2−0), OH (1−0), O 2 (a − X) (0−1), and O 2 (a − X) (0−0) bands. This is the first detection of the first three of these airglow emissions on another planet. These observations provide the most direct observational constraints to date on H, OH, and O 3 , key species in the chemistry of Venus' upper atmosphere. Methods. Airglow emission detected at wavelengths of 1.40−1.49 and 2.6−3.14 µm in limb observations by the Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) on the Venus Express spacecraft is attributed to the OH (2−0) and (1−0) transitions, respectively, and compared to calculations from a photochemical model. Simultaneous limb observations of airglow emission in the O 2 (a − X) (0−0) and (0−1) bands at 1.27 and 1.58 µm, respectively, were used to derive the ratio of the transition probabilities for these bands. Results. The integrated emission rates for the OH (2−0) and (1−0) bands were measured to be 100 ± 40 and 880 ± 90 kR respectively, both peaking at an altitude of 96 ± 2 km near midnight local time for the considered orbit. The measured ratio of the O 2 (a − X) (0−0) and (0−1) bands is 78 ± 8. Conclusions. Photochemical model calculations suggest the observed OH emission is produced primarily via the Bates-Nicolet mechanism, as on the Earth. The observed ratio of the intensities of the O 2 (a − X) (0−0) and (0−1) bands implies the ratio of their transition probabilities is 63 ± 6.

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Scientific goals for the observation of Venus by VIRTIS on ESA/Venus express mission

Cited by 151 publications

References 89 publications

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

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

Saturn Atmospheric Structure and Dynamics

First detection of hydroxyl in the atmosphere of Venus

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