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Non-LTE CO limb emission at in the upper atmosphere of Venus, Mars and Earth: Observations and modeling

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Title: Non-LTE CO limb emission at in the upper atmosphere of Venus, Mars and Earth: Observations and modeling
Authors: Gilli, G.1 gilli@iaa.es, López-Valverde, M.A.1, Funke, B.1, López-Puertas, M.1, Drossart, P.2, Piccioni, G.3, Formisano, V.4
Source: Planetary & Space Science. Aug2011, Vol. 59 Issue 10, p1010-1018. 9p.
Subjects: Planetary atmospheres, Upper atmosphere, Infrared radiation, Remote sensing, Spectrometers, Thermodynamic equilibrium, Vibration (Mechanics), Solar pumps, Venusian atmosphere, Venus (Planet), Martian atmosphere, Mars (Planet)
Abstract: Abstract: We report here on CO limb observations in Mars, Venus and Earth and their model simulations. A comparative study of the CO emission, including the most recent spacecraft observations of the three planets’ atmospheres, has been performed. Strong daytime emissions near have been recently observed in the limb of the upper atmosphere of the three terrestrial planets by the Planetary Fourier Spectrometer on Mars Express (), the Visible and Infrared Thermal Imaging Spectrometer on Venus Express (), and the Michelson Interferometer for Passive Atmosphere Sounding on Envisat (). Those emissions are produced by solar pumping of molecular vibrations and non-local thermodynamic equilibrium (non-LTE) models are used to explain them in a consistent framework for the three atmospheres. The maximum of the emission occurs on Venus between 90 and 110km, on Mars above 60km, and on Earth around 68km. The observations show that the fundamental band dominates the CO non-LTE emission on Earth, while on Venus and Mars the larger contribution comes from the first hot band transition. The main goal of this study is to understand those differences and similarities with the help of theoretical simulations with optical thickness considerations, and compare the capability of space instrumentation for the remote sounding of the atmospheres in this spectral region. [Copyright &y& Elsevier]
Copyright of Planetary & Space Science is the property of Pergamon Press - An Imprint of Elsevier Science and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract. (Copyright applies to all Abstracts.)
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  Data: Non-LTE CO limb emission at in the upper atmosphere of Venus, Mars and Earth: Observations and modeling
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  Data: <searchLink fieldCode="JN" term="%22Planetary+%26+Space+Science%22">Planetary & Space Science</searchLink>. Aug2011, Vol. 59 Issue 10, p1010-1018. 9p.
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  Data: Abstract: We report here on CO limb observations in Mars, Venus and Earth and their model simulations. A comparative study of the CO emission, including the most recent spacecraft observations of the three planets’ atmospheres, has been performed. Strong daytime emissions near have been recently observed in the limb of the upper atmosphere of the three terrestrial planets by the Planetary Fourier Spectrometer on Mars Express (), the Visible and Infrared Thermal Imaging Spectrometer on Venus Express (), and the Michelson Interferometer for Passive Atmosphere Sounding on Envisat (). Those emissions are produced by solar pumping of molecular vibrations and non-local thermodynamic equilibrium (non-LTE) models are used to explain them in a consistent framework for the three atmospheres. The maximum of the emission occurs on Venus between 90 and 110km, on Mars above 60km, and on Earth around 68km. The observations show that the fundamental band dominates the CO non-LTE emission on Earth, while on Venus and Mars the larger contribution comes from the first hot band transition. The main goal of this study is to understand those differences and similarities with the help of theoretical simulations with optical thickness considerations, and compare the capability of space instrumentation for the remote sounding of the atmospheres in this spectral region. [Copyright &y& Elsevier]
– Name: AbstractSuppliedCopyright
  Label:
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  Data: <i>Copyright of Planetary & Space Science is the property of Pergamon Press - An Imprint of Elsevier Science and its content may not be copied or emailed to multiple sites without the copyright holder's express written permission. Additionally, content may not be used with any artificial intelligence tools or machine learning technologies. However, users may print, download, or email articles for individual use. This abstract may be abridged. No warranty is given about the accuracy of the copy. Users should refer to the original published version of the material for the full abstract.</i> (Copyright applies to all Abstracts.)
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        Value: 10.1016/j.pss.2010.07.023
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        Type: general
      – SubjectFull: Upper atmosphere
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      – SubjectFull: Infrared radiation
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