Near‐IR oxygen nightglow observed by VIRTIS in the Venus upper atmosphere

Piccioni, G.; Zasova, L. V.; Migliorini, A.; Drossart, P.; Millour, Ehouarn; Muñoz, A. García; Mills, F. P.; Cardesin-Moinelo, Alessandro

doi:10.1029/2008je003133

Cited by 85 publications

(113 citation statements)

References 55 publications

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“…They found that the peak altitude of the O 2 ð 1 D g Þ volume emission rate is typically located between 95 and 100 km, with a mean value of 97:4 72:5 km. A similar conclusion was reached by Piccioni et al (2009). Observations by VIRTIS in the nadir mode have been used to construct statistical maps of the Venus atmosphere in the O 2 emission band (Gé rard et al, 2008b;Piccioni et al, 2009).…”

Section: Introductionmentioning

confidence: 74%

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Two-dimensional time-dependent model of the transport of minor species in the Venus night side upper atmosphere

Collet

Cox

Gérard

2010

Planetary and Space Science

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a b s t r a c tWe present a numerical tool developed to quantify the role of processes controlling the spatio-temporal distribution of the NO ultraviolet and O 2 ð 1 D g Þ infrared nightglows in the Venus night side upper atmosphere, observed with the VIRTIS and SPICAV instruments on board Venus Express. This numerical tool consists in a two-dimensional chemical-transport time-dependent model which computes in a hypothetical rectangular solving domain the spatio-temporal distributions of the number densities of the four minor species at play in these two nightglow emissions. The coupled nonlinear system of the four partial differential equations, describing the spatio-temporal variations of the minor species, has been solved using a finite volume method with a forward Euler method for the time integration scheme. As an application, we have first simulated a time-constant supply of atoms through the upper boundary of the solving domain. The fluxes are inhomogeneous relative to its horizontal direction, in order to simulate regions of enhanced downward flow of oxygen and nitrogen giving rise to NO and O 2 brightening. Given that these two emissions show large time variations, we have also simulated a timedependent downward flux of O and N atoms. It results from these simulations that the lack of correlation between the NO and O 2 ð 1 D g Þ nightglows largely result from to the coupling between horizontal and vertical transport processes and the very different chemical lifetimes of the two species. In particular, we have quantified the role of each process generating spatio-temporal de-correlations between the NO and O 2 ð 1 D g Þ nightglows.

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Section: Introductionmentioning

confidence: 74%

“…A similar conclusion was reached by Piccioni et al (2009). Observations by VIRTIS in the nadir mode have been used to construct statistical maps of the Venus atmosphere in the O 2 emission band (Gé rard et al, 2008b;Piccioni et al, 2009). These maps indicate the region of enhanced emission is centered on the antisolar point.…”

Section: Introductionmentioning

confidence: 74%

Two-dimensional time-dependent model of the transport of minor species in the Venus night side upper atmosphere

Collet

Cox

Gérard

2010

Planetary and Space Science

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“…It is well adapted to the observation of the O 2 ða 1 DÞ 1.27 lm nightglow in both nadir and limb modes. The horizontal distribution of the emission brightness was studied from nadir VIRTIS observations by Gérard et al (2008b), Piccioni et al (2009) and Soret et al (2012). They found the highest intensity near the antisolar point, with maximum values of respectively 3 MR, 1.2 MR and 1.6 MR (MegaRayleigh) and a mean intensity for the nightside of 1.3 MR, 0.52 MR and 0.50 MR, respectively.…”

Section: Introductionmentioning

confidence: 99%

“…Crisp et al, 1996;Hueso et al, 2008;Krasnopolsky, 2010;Ohtsuki et al, 2005Ohtsuki et al, , 2008Bailey et al, 2008) and space-borne observations from Venus Express have been conducted. The Visible and Infrared Thermal Imaging Spectrometer (VIRTIS) instrument (Drossart et al, 2007;Piccioni et al, 2009) is composed of two spectrometers, including the VIRTIS-M-IR instrument. It is well adapted to the observation of the O 2 ða 1 DÞ 1.27 lm nightglow in both nadir and limb modes.…”

Section: Introductionmentioning

confidence: 99%

The vertical distribution of the Venus NO nightglow: Limb profiles inversion and one-dimensional modeling

Stiepen¹,

Soret²,

Gérard³

et al. 2012

Icarus

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International audienceUltraviolet (UV) spectra of the δ (190-240 nm) and γ (225-270 nm) bands of the nitric oxide (NO) molecule have been measured on the nightside of the atmosphere of Venus with the Spectroscopy for Investigation of Characteristics of the Atmosphere of Venus (SPICAV) instrument on board Venus Express (VEX). Excited NO molecules on the nightside of the planet are created by radiative recombination of O(3P) and N(4S) atoms. The atoms are produced by photodissociation of CO2 and N2 molecules on the dayside and then transported on the nightside by the global circulation. We analyze all nightside limb profiles obtained since 2006 and provide a statistical study of the nitric oxide airglow layer and its variability. We also apply a spatial deconvolution and an Abel inversion method to the limb profiles to retrieve and quantify the volume emission rate distribution and its dependence on several factors. We also show that about 10% of the limb profiles exhibits a secondary peak located above or below the main airglow peak. Furthermore, a one-dimensional chemical-diffusive model is used to simultaneously model the globally averaged NO and O2(a1Δg) airglow vertical distributions using CO2 and O density profiles rooted in VIRTIS and SPICAV observation

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“…VIRTIS-M-IR covers the infrared spectral range from 1 to 5 µm and can observe both in nadir and limb viewing geometries (Drossart et al, 2007;Piccioni et al, 2009). Observations with VIRTIS-M were made between 14 April 2006 (orbit VI0023_01) and 14 October 2008 (orbit VI0907_05).…”

Section: Virtis Observationsmentioning

confidence: 99%

The OH Venus nightglow spectrum: Intensity and vibrational composition from VIRTIS—Venus Express observations

Soret

Gérard

Piccioni

et al. 2012

Planetary and Space Science

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Limb spectra of the OH nightglow emission corresponding to the ∆v=1 and ∆v=2 sequences have been collected with the VIRTIS infrared imaging spectrograph on board Venus Express between April 2006 and October 2008. A detailed statistical analysis shows that the peak intensity and altitude of the two vibrational sequences are significantly correlated, with a mean intensity ratio of the two sequences of 0.38±0.37. The altitude of the maximum of the ∆v=2 emission is located ~1 km lower than ∆v=1. A spectral analysis shows that the Δv=1 sequence is composed at 44.6% by the (1-0) band, 9.3% by the (3-2) band and 7.1% by the (4-3) band. The Δv=2 emission is best fitted if solely including the (2-0) band.A non-LTE model of OH vibrational population by the O 3 + H reaction including radiative and collisional relaxation has been used to compare the expected spectral distribution, the altitude of the emission peak and the emission rate under different assumptions on the quenching processes to those observed with VIRTIS. The adopted carbon dioxide, atomic 2 oxygen and ozone densities are based on recent Venus Express remote sensing measurements.We find that the "sudden death" quenching scheme by CO 2 produces inadequate spectral distribution between the various bands and insufficient airglow brightness. Instead, the observed spectral distribution and the total emission intensity are reasonably well reproduced with the single quantum jump model, a O density profile peaking at 103.5 km with a maximum value of 1.9x10 11 cm -3 , a O 3 density profile peaking at 5.8x10 6 cm -3 at 96.5 km and a H density profile close to 10 8 cm -3 between 90 and 120 km, in agreement with several photochemical models.• The infrared OH Meinel bands have been observed by VIRTIS on board Venus Express.• The ∆v=1 and ∆v=2 sequences are significantly correlated in altitude and intensity.• Most of the population is in the lower vibrational levels.• A non-LTE model was developed using O, O 3 and CO 2 densities from VEX measurements.• Observations are reproduced with these densities and a single quantum jump model.

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Near‐IR oxygen nightglow observed by VIRTIS in the Venus upper atmosphere

Cited by 85 publications

References 55 publications

Two-dimensional time-dependent model of the transport of minor species in the Venus night side upper atmosphere

Two-dimensional time-dependent model of the transport of minor species in the Venus night side upper atmosphere

The vertical distribution of the Venus NO nightglow: Limb profiles inversion and one-dimensional modeling

The OH Venus nightglow spectrum: Intensity and vibrational composition from VIRTIS—Venus Express observations

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