The Chemical Composition of the Venus Atmosphere Based on the Data of the Interplanetary Station Venera 4

Vinogradov, A. P.; Surkov, U. A.; Florensky, C. P.

doi:10.1175/1520-0469(1968)025<0535:tccotv>2.0.co;2

Cited by 47 publications

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“…The scientific basis of the RO technique was developed in the 1960s for soundings of the atmospheric parameters of the other planets in our solar system (e.g., Kliore et al 1965Kliore et al , 1967Vinogradov et al 1968;Fjeldbo andEshleman 1968,1969). Approximately at the same time Fischbach (1965) and Lusignan et al (1969) proposed the use of the same technique for the sounding of the Earth's atmosphere.…”

Section: Radio Occultation Measurementmentioning

confidence: 99%

Prospects of the EPS GRAS Mission For Operational Atmospheric Applications

Luntama¹,

Kirchengast²,

Borsche³

et al. 2008

Bulletin of the American Meteorological Society

104

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Section: Radio Occultation Measurementmentioning

confidence: 99%

Prospects of the EPS GRAS Mission For Operational Atmospheric Applications

Luntama¹,

Kirchengast²,

Borsche³

et al. 2008

Bulletin of the American Meteorological Society

104

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“…At the two levels P =0.6 and P = 2.0 arm, the molar fraction of www.annualreviews.org/aronline Annual Reviews water was found to be in the range 0.1-1.0% (Vinogradov, Surkov Florensky 1968, Avduevsky, Marov & Rozhdestvensky 1970. However, Lewis (1969) has argued that the change in electrical conductivity is due the presence of concentrated aqueous solutions of HC1 in the Venus clouds, and that the mole fraction of water in the atmosphere is only 10 -4.…”

Section: Carbon Dioxide--thementioning

confidence: 99%

“…only direct sampling of a planetary atmosphere other than the Earth's was carried out on the Soviet entry probes Venera 5, and 6 (Vinogradov, Surkov & Florensky 1968, Avduevsky, Marov Rozhdestvensky 1970. Data on the composition of the Venus atmosphere were obtained at two levels, P=0.6 and 2.0 atm, respectively, where _P is total atmospheric pressure.…”

Section: Carbon Dioxide--thementioning

confidence: 99%

The Atmospheres of Mars and Venus

Ingersoll¹,

Leovy²

1971

Annu. Rev. Astron. Astrophys.

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“…Convincing proof for the existence of water vapor has, however, come from the measurements of the space probes, Venera 4, 5, 6 and Mariner V, in the atmosphere of Venus. Venera 4 indicated 1 to 8 mg liter" 1 of water (Vinogradov et al, 1968) whereas Venera 5 and 6 ('Venera 5 and 6', 1969) gave 4 to 11 at 0.6 atm total pressure and 25 °C. Observations of Mariner V also indicated small amounts.…”

Section: Introductionmentioning

confidence: 96%

Water on Venus?

Libby

Corneil

1971

Symp. - Int. Astron. Union

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Abstract. It is proposed that Venus may have polar seas which are acidic and thus cannot precipi tate calcium carbonate. This leaves the carbon dioxide in the atmosphere. The argument is that the great equatorial land masses always have been too hot for liquid water and thus could not be weathered to give the sea salts necessary to form the precipitate. The action of steam on rocks is to liberate acids which are volatile and would dissolve in the polar seas. The volcanic vapors issuing in the early times consisting mainly of water and carbon dioxide would have begun polar seas at once since the expected equatorial (black body) surface temperature of the bare planet is too high (464 K) due to proximity of the sun. The accumulation of carbon dioxide in the atmosphere would have ensured the continued increase of the temperature due to the greenhouse effect. On earth, on the contrary, condensation over most of the planetary surface probably was possible from the beginning. Liquid water, ice-weathering, and river transport of salts to the seas all probably occurred from the beginning.As the pressure at the surface probably approximates 100 atm (Venera 5 and 6) we can expect the polar seas to be below the boiling point although possibly hot. An isothermal layer of some thickness is naturally established over liquid water heated by infrared from above. Evaporation and condensation to form rain constitutes an efficient heat transport mechanism. Such a layer naturally would move toward lower latitude carrying moisture which then will rise and eventually move poleward in the high atmosphere causing rain and possibly the planet wide cloud cover. The atmosphere containing volatiles such as hydrochloric and hydrofluoric and sulfurous and sulfuric acids as well as carbon dioxide will form clouds which might be expected to consist of concentrated acid solutions. The main rain over the poles probably falls from altitudes well below the cloud top seen from earth. It is possible that the Venus clouds seen from earth are non aqueous just as our stratosphere carries dust clouds apparently of ammonium sulfate. At the moment it is very difficult to decide between these alternatives.In the more polar regions the seas might conceivably be as cool as 50 °C.

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The Chemical Composition of the Venus Atmosphere Based on the Data of the Interplanetary Station Venera 4

Cited by 47 publications

References 0 publications

Prospects of the EPS GRAS Mission For Operational Atmospheric Applications

Prospects of the EPS GRAS Mission For Operational Atmospheric Applications

The Atmospheres of Mars and Venus

Water on Venus?

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