The distribution of carbon monoxide in the lower atmosphere of Venus

Cotton, Daniel V.; Bailey, Jeremy; Crisp, David; Meadows, V. S.

doi:10.1016/j.icarus.2011.05.020

Cited by 43 publications

(33 citation statements)

References 43 publications

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“…Cotton et al . [] also found evidence of a higher amount of CO in the north than the south. Third, our time series of data suggests that the mixing ratio of CO near the downwelling branch of the southern Hadley cell may increase between 1 March and 3 March by roughly 14%.…”

Section: Measurements and Discussionmentioning

confidence: 92%

“…In Cotton et al . [], although more CO was observed in the north than the south over the whole data set, annual time variable trends may be present. Maps produced in July 2004 appear to have more CO in the north than the south, but maps from December 2005 seem to have roughly equal amounts in each hemisphere (11 December is an exception which may have more CO in the south).…”

Section: Measurements and Discussionmentioning

confidence: 99%

“…Here we report our CO abundance measurements at 35 km and adopt the nominal CO atmospheric profile of Cotton et al . [].…”

Section: Measurements and Discussionmentioning

confidence: 99%

“…Figures 9 and 10 in Cotton et al . [] display these measurements. Taken together with previous studies, our measurements between 2009 and 2010 may be consistent with an oscillatory hemispherical dichotomy, but more work must be done to understand the cause of the dichotomy and the timescales and mechanisms involved in its apparent reversals.…”

Section: Measurements and Discussionmentioning

confidence: 99%

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Spatially resolved measurements of H₂O, HCl, CO, OCS, SO₂, cloud opacity, and acid concentration in the Venus near-infrared spectral windows

Arney

Meadows

Crisp

et al. 2014

J. Geophys. Res. Planets

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130

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Section: Measurements and Discussionmentioning

confidence: 92%

Section: Measurements and Discussionmentioning

confidence: 99%

“…Here we report our CO abundance measurements at 35 km and adopt the nominal CO atmospheric profile of Cotton et al . [].…”

Section: Measurements and Discussionmentioning

confidence: 99%

Section: Measurements and Discussionmentioning

confidence: 99%

See 2 more Smart Citations

Spatially resolved measurements of H₂O, HCl, CO, OCS, SO₂, cloud opacity, and acid concentration in the Venus near-infrared spectral windows

Arney

Meadows

Crisp

et al. 2014

J. Geophys. Res. Planets

Self Cite

130

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“…In addition to CO 2 , we are considering molecular nitrogen (X N 2 = 3.5%), molecular and atomic oxygen (O 2 and O i), carbon monoxide (CO), water (H 2 O), and sulfur dioxide (SO 2 ). The mixing ratio profiles for CO, SO 2 , and H 2 O are extrapolated from the values from Cotton et al (2011), de Bergh et al (2006, respectively. Mixing ratios of O 2 and O i are considered to be nonzero only in the upper atmosphere, where these species are produced; there, their mixing ratio profiles follow those calculated by Gronoff et al (2008).…”

Section: Atmospherementioning

confidence: 99%

Transmission spectrum of Venus as a transiting exoplanet

Ehrenreich

Vidal‐Madjar

Widemann

et al. 2011

A&A

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On 5-6 June 2012, Venus will be transiting the Sun for the last time before 2117. This event is an unique opportunity to assess the feasibility of the atmospheric characterisation of Earth-size exoplanets near the habitable zone with the transmission spectroscopy technique and provide an invaluable proxy for the atmosphere of such a planet. In this letter, we provide a theoretical transmission spectrum of the atmosphere of Venus that could be tested with spectroscopic observations during the 2012 transit. This is done using radiative transfer across Venus' atmosphere, with inputs from in-situ missions such as Venus Express and theoretical models. The transmission spectrum covers a range of 0.1-5 μm and probes the limb between 70 and 150 km in altitude. It is dominated in UV by carbon dioxide absorption producing a broad transit signal of ∼20 ppm as seen from Earth, and from 0.2 to 2.7 μm by Mie extinction (∼5 ppm at 0.8 μm) caused by droplets of sulfuric acid composing an upper haze layer above the main deck of clouds. These features are not expected for a terrestrial exoplanet and could help discriminating an Earth-like habitable world from a cytherean planet.

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Simulations of the latitudinal variability of CO‐like and OCS‐like passive tracers below the clouds of Venus using the Laboratoire de Météorologie Dynamique GCM

Marcq

Lebonnois

2013

JGR Planets

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[1] The lower atmosphere of Venus below the clouds is a transitional region between the relatively calm lowermost scale height and the superrotating atmosphere in the cloud region and above. Any observational constraint is then welcome to help in the development of general circulation models of Venus, a difficult task considering the thickness of its atmosphere. Starting from a state-of-the-art 3-D Venus General Circulation Model (GCM), we have included passive tracers in order to investigate the latitudinal variability of two minor gaseous species, carbonyl sulfide (OCS) and carbon monoxide (CO), whose vertical profiles and mixing ratios are known to vary with latitude between 30 and 40 km. The relaxation to chemical equilibrium is crudely parametrized through a vertically uniform time scale . A satisfactory agreement with available observations is obtained with 10 8 s . CO . 5 10 8 s and 10 7 s . OCS . 10 8 s. These results, in addition to validating the general circulation below the clouds, are also helpful in characterizing the chemical kinetics of Venus' atmosphere. This complements the much more sophisticated chemical models which focus more on thermodynamical equilibrium.Citation: Marcq, E., and S. Lebonnois (2013), Simulations of the latitudinal variability of CO-like and OCS-like passive tracers below the clouds of Venus using the Laboratoire de Météorologie Dynamique GCM,

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The distribution of carbon monoxide in the lower atmosphere of Venus

Cited by 43 publications

References 43 publications

Spatially resolved measurements of H₂O, HCl, CO, OCS, SO₂, cloud opacity, and acid concentration in the Venus near-infrared spectral windows

Spatially resolved measurements of H₂O, HCl, CO, OCS, SO₂, cloud opacity, and acid concentration in the Venus near-infrared spectral windows

Transmission spectrum of Venus as a transiting exoplanet

Simulations of the latitudinal variability of CO‐like and OCS‐like passive tracers below the clouds of Venus using the Laboratoire de Météorologie Dynamique GCM

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The distribution of carbon monoxide in the lower atmosphere of Venus

Cited by 43 publications

References 43 publications

Spatially resolved measurements of H2O, HCl, CO, OCS, SO2, cloud opacity, and acid concentration in the Venus near-infrared spectral windows

Spatially resolved measurements of H2O, HCl, CO, OCS, SO2, cloud opacity, and acid concentration in the Venus near-infrared spectral windows

Transmission spectrum of Venus as a transiting exoplanet

Simulations of the latitudinal variability of CO‐like and OCS‐like passive tracers below the clouds of Venus using the Laboratoire de Météorologie Dynamique GCM

Contact Info

Product

Resources

About

Spatially resolved measurements of H₂O, HCl, CO, OCS, SO₂, cloud opacity, and acid concentration in the Venus near-infrared spectral windows

Spatially resolved measurements of H₂O, HCl, CO, OCS, SO₂, cloud opacity, and acid concentration in the Venus near-infrared spectral windows