Water vapour in the lower atmosphere of Venus: a new analysis of optical spectra measured by entry probes

Ignatiev, Nikolay; Мороз, В. І.; Moshkin, B. E.; Ekonomov, A. P.; Gnedykh, V. I.; Grigoriev, Аlexey; Khatuntsev, I.

doi:10.1016/s0032-0633(96)00143-2

Cited by 67 publications

(37 citation statements)

References 31 publications

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“…These calculations allowed Marov et al (1984) to estimate the water vapor profile in the atmosphere of Venus independently of spectroscopic measurements in the visible range. The estimates were later confirmed in (Ignat'ev et al , 1997), where the water profile was retrieved from the spectroscopic data more accurately. Meanwhile, for any reasonable water vapor concentrations, the flux calculated at heights below 30 km is always larger than the observed flux.…”

Section: Introductionmentioning

confidence: 80%

“…5. The coefficients of aerosol extinction were defined by analyzing the Fourier spectrometry of the atmosphere of Venus obtained during the Venera-15 mission (Zasova et al, 1996), taking into account the entry probe data (Ignat'ev et al, 1997). The relatively low single-scattering albedo in the thermal range indicates that aerosol scattering may be neglected.…”

Section: Optical Properties Of the Cloud Layermentioning

confidence: 99%

“…The downward solar flux decreases from ~160 W/m 2 directly below the cloud layer to ~16 W/m 2 near the surface. The spectral measurements in the visible range performed by the Venera-11, Venera-12, Venera-13 , and Venera-14 landers resulted in an evaluation of the water vapor content (Moroz et al , 1983;Ignat'ev et al , 1997). AFANASENKO, RODIN The NASA Pioneer Venus entry probes carried out radiometric measurements of the thermal radiation fluxes in the Venusian atmosphere below the cloud layer.…”

Section: Introductionmentioning

confidence: 99%

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The Effect of Collisional Line Broadening on the Spectrum and Fluxes of Thermal Radiation in the Lower Atmosphere of Venus

Afanasenko

Rodin

2005

Sol Syst Res

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The absorption spectrum and thermal radiation fluxes are calculated for the lower atmosphere of Venus in the far-wing approximation based on the theory of the collisional broadening of spectral lines. The results are in good agreement with the available experimental data. An outgoing thermal radiation flux is about 2.6 W/m 2 near the planetary surface. This indicates that free convection significantly contributes to the thermal balance of the lower troposphere. The fluxes obtained in this study were compared to those calculated on the basis of empirical models of the spectral line profile. It was shown that the far wings of the CO 2 lines considerably affect the radiative transfer in the transparency windows. This effect becomes weaker when the contribution of the absorption of minor constituents, primarily water vapor, increases. The profiles of absorption lines of minor constituents do not influence the thermal radiation fluxes.

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Section: Introductionmentioning

confidence: 80%

Section: Optical Properties Of the Cloud Layermentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Effect of Collisional Line Broadening on the Spectrum and Fluxes of Thermal Radiation in the Lower Atmosphere of Venus

Afanasenko

Rodin

2005

Sol Syst Res

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“…Other processes dominate below 47-50 km. The radiation extinction at λ > 0.66 µ m is mainly due to absorption by ëé 2 and ç 2 é molecules (the analysis of the spectra received from the Venera-11 , -13 , and -14 probes in this range allowed the vertical profile of the water vapor content in the atmosphere of Venus to be obtained (Ignat'ev et al , 1997)). The major extinction process at λ < 0.67 µ m is the molecular scattering accompanied by the true absorption that will be considered in detail below.…”

Section: Introductionmentioning

confidence: 99%

“…The data from the Venera-11 probe are presented. The spectrometer resolution (at a level of 0.5) shown in the plot for the visible ∆ and infrared ∆ wavelength ranges (Ekonomov et al, 1979;Moroz et al, 1983) allowed the absorption bands of gaseous ëé 2 and ç 2 é to be identified rather easily (see, e.g., Moroz et al, 1979b;Moshkin et al, 1983;Ignat'ev et al, 1997).…”

Section: Introductionmentioning

confidence: 99%

A New Analysis of the Spectra Obtained by the Venera Missions in the Venusian Atmosphere. I. The Analysis of the Data Received from the Venera-11 Probe at Altitudes Below 37 km in the 0.44–0.66 µm Wavelength Range

et al. 2005

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The processes of the solar radiation extinction in deep layers of the Venus atmosphere in a wavelength range from 0.44 to 0.66 µ m have been considered. The spectra of the solar radiation scattered in the atmosphere of Venus at various altitudes above the planetary surface measured by the Venera-11 entry probe in December 1978 are used as observational data. The problem of the data analysis is solved by selecting an atmospheric model; the discrete-ordinate method is applied in calculations. For the altitude interval from 2-10 km to 36 km, the altitude and spectral dependencies of the volume coefficient of true absorption have been obtained. At altitudes of 3-19 km, the spectral dependence is close to the wavelength dependence of the absorption cross section of S 3 molecules, whence it follows that the mixing ratio of this sulfur allotrope increases with altitude from 0.03 to 0.1 ppbv.

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Winds in the Middle Cloud Deck From the Near‐IR Imaging by the Venus Monitoring Camera Onboard Venus Express

et al. 2017

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For more than 8 years the Venus Monitoring Camera (VMC) onboard the Venus Express orbiter performed continuous imaging of the Venus cloud layer in UV, visible and near‐IR filters. We applied the correlation approach to sequences of the near‐IR images at 965 nm to track cloud features and determine the wind field in the middle and lower cloud (49–57 km). From the VMC images that spanned from December of 2006 through August of 2013 we derived zonal and meridional components of the wind field. In low‐to‐middle latitudes (5–65°S) the velocity of the retrograde zonal wind was found to be 68–70 m/s. The meridional wind velocity slowly decreases from peak value of +5.8 ± 1.2 m/s at 15°S to 0 at 65–70°S. The mean meridional speed has a positive sign at 5–65°S suggesting equatorward flow. This result, together with the earlier measurements of the poleward flow at the cloud tops, indicates the presence of a closed Hadley cell in the altitude range 55–65 km. Long‐term variations of zonal and meridional velocity components were found during 1,200 Earth days of observation. At 20° ± 5°S the zonal wind speed increases from −67.18 ± 1.81 m/s to −77.30 ± 2.49 m/s. The meridional wind gradually increases from +1.30 ± 1.82 m/s to +8.53 ± 2.14 m/s. Following Bertaux et al. (2016) we attribute this long‐term trend to the influence from the surface topography on the dynamical process in the atmosphere via the upward propagation of gravity waves that became apparent in the VMC observations due to slow drift of the Venus Express orbit over Aphrodite Terra.

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Water vapour in the lower atmosphere of Venus: a new analysis of optical spectra measured by entry probes

Cited by 67 publications

References 31 publications

The Effect of Collisional Line Broadening on the Spectrum and Fluxes of Thermal Radiation in the Lower Atmosphere of Venus

The Effect of Collisional Line Broadening on the Spectrum and Fluxes of Thermal Radiation in the Lower Atmosphere of Venus

A New Analysis of the Spectra Obtained by the Venera Missions in the Venusian Atmosphere. I. The Analysis of the Data Received from the Venera-11 Probe at Altitudes Below 37 km in the 0.44–0.66 µm Wavelength Range

Winds in the Middle Cloud Deck From the Near‐IR Imaging by the Venus Monitoring Camera Onboard Venus Express

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