Spectrum of the Venus day sky

Мороз, В. І.; Golovin, Yu. M.; Ekonomov, A. P.; Moshkin, B. E.; Parfentev, N. A.; Sanko, N. F.

doi:10.1038/284243a0

Cited by 40 publications

(18 citation statements)

References 6 publications

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“…Vertical profile of H20 in the atmosphere of Venus. 1 -V4, 2 -V5 (electrolytic method, the interval of probable humidity values is limited by full lines), 3 -V5 (manometric method), 4 -V6, 5 -ground-based observations (limits of variability are shown, , 6 -the model being in the best agreement with the optical spectrometry in the Vll data (Moroz et al, 1979b), 7 -gaseous chromatograph (Oyama et aL, 1979b(Oyama et aL, , 1980. Results obtained on V4, 5, and 6 are given according to Andrejchikov (1978).…”

Section: H20mentioning

confidence: 98%

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The atmosphere of Venus

Мороз

1981

Space Sci Rev

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The investigations of Venus take a special position in planetary researches. It was just the atmosphere of Venus where first measurements m situ were carried out by means of the equipment delivered by a space probe (Venera 4, 1967). Venus appeared to be the first neighbor planet whose surface had been seen by us in the direct nearness made possible by means of the phototelevision device (Venera 9 and Venera 10, 1975).The reasons for the high interest in this planet are very simple. This planet is like the Earth by its mass, size and amount of energy obtained from the Sun and at the same time it differs sharply by the character of its atmosphere and climate.

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Section: H20mentioning

confidence: 98%

“…The experiment was much improved on the Vll and V12. A spectrophotometer with continuous scanning of the spectrum in the region 4500-12 000 ~ was used there (Moroz et al, 1979a(Moroz et al, , b, 1980Ekonomov et al, 1979). Examples of measured spectra are presented in Figure 9.…”

Section: H20mentioning

confidence: 99%

The atmosphere of Venus

Мороз

1981

Space Sci Rev

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“…The Venera 11 and 12 descent probes carried scanning infrared spectrophotometers that recorded the spectrum of the Venus daytime sky. Synthetic spectra constructed by Moroz et al (1980) indicated that the H20 abundance is about 20 ppm near the surface increasing to 200 ppm in the clouds. From measurements made by the net flux radiometers on the four PV probes, Revercomb et al (1985) have reported that the water abundance below the clouds varies with latitude, with mixing ratio of 20 to 50 ppm at 60 ~ increasing to about 500 ppm at the equator.…”

Section: H20 Densitiesmentioning

confidence: 99%

Structure, luminosity, and dynamics of the Venus thermosphere

Fox

Bougher

1991

Space Sci Rev

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We review here observations and models related to the chemical and thermal structures, airglow and auroral emissions and dynamics of the Venus thermosphere, and compare empirical models of the neutral densities based in large part on in situ measurements obtained by the Pioneer Venus spacecraft.Observations of the intensities of emissions are important as a diagnostic tool for understanding the chemical and physical processes taking place in the Venus thermosphere. Measurements, ground-based and from rockets, satellites, and spacecraft, and model predictions of atomic, molecular and ionic emissions, are presented and the most important sources are elucidated. Coronas of hot hydrogen and hot oxygen have been observed to surround the terrestrial planets. We discuss the observations of and production mechanisms for the extended exospheres and models for the escape of lighter species from the atmosphere. Over the last decade and a half, models have attempted to explain the unexpectedly cold temperatures in the Venus thermosphere; recently considerable progress has been made, although some controversies remain. We review the history of these models and discuss the heating and cooling mechanisms that are presently considered to be the most important in determining the thermal structure. Finally, we discuss major aspects of the circulation and dynamics of the thermosphere: the sub-solar to anti-solar circulation, superrotation, and turbulent processes.

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“…1 and 7c), where the absorption is very likely caused by other constituents of the Venusian atmosphere that have not been identified reliably so far. Among the absorbers in this spectral range, there might be such agents as Cl 2 (Pollack et al , 1980), Br 2 , NO 2 , and others; but the most probable candidate is gaseous sulfur (Moroz et al , 1979a(Moroz et al , , 1980Krasnopol'skii and Parshev, 1979), specifically, its allotropes S 3 and S 4 (San 'ko, 1980;Moroz et al , 1981Moroz et al , , 1983.…”

Section: Introductionmentioning

confidence: 97%

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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Spectrum of the Venus day sky

Cited by 40 publications

References 6 publications

The atmosphere of Venus

The atmosphere of Venus

Structure, luminosity, and dynamics of the Venus thermosphere

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

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