Distribution of the O<sub>2</sub> infrared nightglow observed with VIRTIS on board Venus Express

Gérard, Jean‐Claude; Saglam, Adem; Piccioni, G.; Drossart, P.; Cox, Cédric; Erard, S.; Hueso, R.; Sánchez‐Lavega, A.

doi:10.1029/2007gl032021

Cited by 57 publications

(94 citation statements)

References 22 publications

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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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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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“…The non-LTE emission in the O 2 band at 1.27 μm that originates from the recombination of oxygen atoms on the night side peaks at around midnight ( Fig. 11) (Drossart et al, 2007b;Gerard et al, 2008). Also the temperature maximum observed on the night side was attributed to adiabatic heating in the subsiding branch of the thermospheric solar to anti-solar circulation (Fig.…”

Section: Summary Of the Resultsmentioning

confidence: 98%

Venus express: Highlights of the nominal mission

et al. 2009

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-Venus Express is the first European (ESA) mission to the planet Venus. Its main science goal is to carry out a global survey of the atmosphere, the plasma environment, and the surface of Venus from orbit. The payload consists of seven experiments. It includes a powerful suite of remote sensing imagers and spectrometers, instruments for in-situ investigation of the circumplanetary plasma and magnetic field, and a radio science experiment. The spacecraft, based on the Mars Express bus modified for the conditions at Venus, provides a versatile platform for nadir and limb observations as well as solar, stellar, and radio occultations. In April 2006 Venus Express was inserted in an elliptical polar orbit around Venus, with a pericentre height of ~250 km and apocentre distance of ~66000 km and an orbital period of 24 hours. orbit. In particular, fundamental problems in the fields of atmospheric structure and composition, morphology and distribution of clouds and hazes, atmospheric dynamics, properties of plasma and magnetic field, and escape processes, are all addressed by the Venus Express observations. These investigations will shed light on the current climate of Venus, will make it possible to reconstruct the evolutionary path of our sister planet, and will make significant contribution to the field of comparative planetology.The Venus Express payload consists to a great extent of the instruments inherited from the Mars Express and Rosetta missions, which were found to be quite suitable for making a breakthrough in Venus studies (Titov et al., 2001). The payload core consists of a suite of imagers and spectrometers, combining wide spectral range from the UV to the thermal IR. Broad band context imaging and high spectral resolution makes the mission payload the most capable remote sensing package ever flown to Venus. This suite is complemented by a radio science experiment to investigate the structure of the neutral atmosphere and ionosphere. Two experiments monitor the ambient magnetic field and study the plasma environment and escape processes.

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“…At Venus, NO UV nightglow, O 2 ( 1 g ) 1.27-µm nightglow, and O 2 400-800 nm nightglow intensity distributions and their temporal variability are being used to constrain GCMs and uncover the thermospheric general circulation patterns and wind magnitude responsible. Pioneer Venus, Venus Express, and ground based nightglow observations have all contributed to this process of tracing Venus thermospheric wind patterns (see reviews by Lellouch et al 1997;Bougher et al , 2006aGerard et al 2008). At Mars, recent Mars Express SPICAM observations of NO nightglow emissions at high latitudes (Bertaux et al 2005) plus several winter polar warming measurements from aerobraking missions (e.g.…”

Section: Nightglowmentioning

confidence: 95%

“…A measurement of the absolute value of this yield in CO 2 is also greatly needed to further constrain model simulations. The interpretation of recent Venus Express O 2 ( 1 g ) 1.27-µm nightglow distributions (Gerard et al 2008) will be greatly advanced by such new laboratory measurements.…”

Section: Nightglowmentioning

confidence: 98%