AustralieFrV1, Main, Exploration, bibRecord, 005836

The distribution of carbon monoxide in the lower atmosphere of Venus

Identifieur interne : 005836 ( Main/Exploration ); précédent : 005835; suivant : 005837

The distribution of carbon monoxide in the lower atmosphere of Venus

Auteurs : Daniel V. Cotton [Australie] ; Jeremy Baileya [États-Unis] ; D. Crisp [États-Unis] ; V. S. Meadows [États-Unis]

Source :

Icarus : (New York, N.Y. 1962) [ 0019-1035 ] ; 2012.

RBID : Pascal:12-0146111

Descripteurs français

Pascal (Inist)
- Planète Vénus, Spectrométrie IR proche, Bande absorption, Transfert radiatif, Modèle, Rapport mélange, Abondance, Modélisation, Haute atmosphère, Dynamique, Système solaire.

English descriptors

KwdEn :
- Absorption band, Abundance, Dynamics, Mixing ratio, Modelling, Models, Near infrared spectrometry, Radiative transfer, Solar system, Upper atmosphere, Venus planet.

Abstract

We have obtained spatially resolved near-infrared spectroscopy of the Venus nightside on 15 nights over three observing seasons. We use the depth of the CO absorption band at 2.3 μm to map the two-dimensional distribution of CO across both hemispheres. Radiative transfer models are used to relate the measured CO band depth to the volume mixing ratio of CO. The results confirm previous investigations in showing a general trend of increased CO abundances at around 60° latitude north and south as compared with the equatorial regions. Observations taken over a few nights generally show very similar CO distributions, but significant changes are apparent over longer periods. In past studies it has been assumed that the CO latitudinal variation occurs near 35 km altitude, at which K-band sensitivity to CO is greatest. By modeling the detailed spectrum of the excess CO at high latitudes we show that it occurs at altitudes around 45 km, much higher than has previously been assumed, and that there cannot be significant contribution from levels of 36 km or lower. We suggest that this is most likely due to downwelling of CO-rich gas from the upper atmosphere at these latitudes, with the CO being removed by around 40 km through chemical processes such as the reaction with SO₃.

Affiliations:

Links toward previous steps (curation, corpus...)

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to stream Main, to step Curation: 005836

Le document en format XML

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<front><div type="abstract" xml:lang="en">We have obtained spatially resolved near-infrared spectroscopy of the Venus nightside on 15 nights over three observing seasons. We use the depth of the CO absorption band at 2.3 μm to map the two-dimensional distribution of CO across both hemispheres. Radiative transfer models are used to relate the measured CO band depth to the volume mixing ratio of CO. The results confirm previous investigations in showing a general trend of increased CO abundances at around 60° latitude north and south as compared with the equatorial regions. Observations taken over a few nights generally show very similar CO distributions, but significant changes are apparent over longer periods. In past studies it has been assumed that the CO latitudinal variation occurs near 35 km altitude, at which K-band sensitivity to CO is greatest. By modeling the detailed spectrum of the excess CO at high latitudes we show that it occurs at altitudes around 45 km, much higher than has previously been assumed, and that there cannot be significant contribution from levels of 36 km or lower. We suggest that this is most likely due to downwelling of CO-rich gas from the upper atmosphere at these latitudes, with the CO being removed by around 40 km through chemical processes such as the reaction with SO<sub>3</sub>
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The distribution of carbon monoxide in the lower atmosphere of Venus

The distribution of carbon monoxide in the lower atmosphere of Venus

Source :

Descripteurs français

English descriptors

Abstract

Links toward previous steps (curation, corpus...)

Le document en format XML

Pour manipuler ce document sous Unix (Dilib)

Pour mettre un lien sur cette page dans le réseau Wicri