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

Maiorov, B. S.; Ignat’ev, N. I.; Мороз, В. І.; Zasova, L. V.; Moshkin, B. E.; Khatuntsev, I.; Ekonomov, A. P.

doi:10.1007/s11208-005-0042-1

Cited by 35 publications

(10 citation statements)

References 26 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The retrieval results were f S 3 = 11 ± 3 pptv at 3-10 km, f S 3 = 18 ± 3 pptv at 10-19 km, f S 4 = 4 ± 4 pptv at 3-10 km, and f S 4 = 6 ± 2 pptv at 10-19 km. Both species show a rapid decrease above 19 km (Maiorov et al 2005).…”

Section: Sulphur-bearing Species: So 2 H 2 So 4 Smentioning

confidence: 94%

See 1 more Smart Citation

Composition and Chemistry of the Neutral Atmosphere of Venus

Marcq¹,

Mills²,

Sandor³

et al. 2017

Space Sci Rev

108

117

View full text Add to dashboard Cite

International audienceThis paper deals with the composition and chemical processes occurring in the neutral atmosphere of Venus. Since the last synthesis, observers as well as modellers have emphasised the spatial and temporal variability of minor species, going beyond a static and uniform picture that may have prevailed in the past. The outline of this paper acknowledges this situation and follows closely the different dimensions along which variability in composition can be observed: vertical, latitudinal, longitudinal, temporal. The strong differences between the atmosphere below and above the cloud layers also dictate the structure of this paper. Observational constraints, obtained from both Earth and Venus Express, as well as 1D, 2D and 3D models results obtained since 1997 are also extensively referred and commented by the authors. An non-exhaustive list of topics included follows: modelled and observed latitudinal and vertical profiles of CO and OCS below the clouds of Venus; vertical profiles of CO and SO2 above the clouds as observed by solar occultation and modelled; temporal and spatial variability of sulphur oxides above the clouds. As a conclusion, open questions and topics of interest for further studies are discussed

show abstract

Section: Sulphur-bearing Species: So 2 H 2 So 4 Smentioning

confidence: 94%

“…Re-analysis of in situ scattered sunlight in the visible range obtained during Venera 11 probe descent was performed by Maiorov et al (2005). They found new estimates of the S 3 mixing ratio in the 3 to 19 km altitude range, with a volume mixing ratio increasing with increasing altitude from 0.03 to 0.1 ppbv.…”

Section: Sulphur-bearing Species: So 2 H 2 So 4 Smentioning

confidence: 99%

Composition and Chemistry of the Neutral Atmosphere of Venus

Marcq¹,

Mills²,

Sandor³

et al. 2017

Space Sci Rev

108

117

View full text Add to dashboard Cite

show abstract

“…Note that S 3 has been tentatively identified by UV data from Venera 14, and S x is a leading candidate for the unidentified UV and blue absorber [see Mills et al, 2007, sections 3 and 6]. The amount quoted for S 3 by Maiorov et al [2005] is 0.03 to 0.1 ppb. Bertaux et al [1986] reported 5 to 25 ppmv of S 8 from 25 to 45 km from analysis of UV data obtained by Venera 11 and 12.…”

Section: Appendix A: Hypothesis Of An Innovative Chemical Cyclementioning

confidence: 99%

Evidence for carbonyl sulfide (OCS) conversion to CO in the lower atmosphere of Venus

et al. 2009

View full text Add to dashboard Cite

[1] The chemical regimes in the atmosphere of Venus vary from photochemistry in the middle atmosphere to thermal equilibrium chemistry in the lower atmosphere and the surface. Many chemical cycles have been proposed, but few details about these cycles are fully verified by comparison between observations and modeling. Recent high-quality data of carbonyl sulfide (OCS) and CO from ground-based and Venus Express observations provide a unique opportunity to test our understanding of chemistry and transport in the lower atmosphere of Venus. The spatial distributions of OCS and CO in the atmosphere reflect a sensitive balance between chemistry and transport. On the basis of our updated photochemical model and winds from Lee et al.'s (2007) general circulation model, we study the chemistry and transport in a simplified two-dimensional chemistry-transport model. OCS is produced by heterogeneous reactions on the surface; the middle atmosphere is a net sink for OCS. The combination of data and modeling provides strong evidence for the loss of OCS by conversion to CO. The detailed chemical mechanism is currently unknown, although a number of speculations have been proposed. The sensitivity of the distributions of OCS and CO to model parameters is reported.

show abstract

“…h 2 S was reported by Pioneer Venus below 20 km [Hoffman et al, 1980], but it was never confirmed by an independent measurement and the reported value is at least an order of magnitude larger than would be expected from thermochemical equilibrium calculations [Fegley et al, 1997b]. Strong absorption in spectrophotometer data from VEnErA 11, 12, 13 and 14 at 450-600 nm between 10 and 30 km has been attributed most commonly to gaseous elemental sulfur (polysulfur, S x ) [Moroz et al, 1979;Sanko, 1980;Krasnopolsky, 1987;Maiorov et al, 2005] and there is good agreement between calculated and observed Venera-11 spectra at 3-19 km assuming the abundance of S 3 increases with altitude from 0.03 ppbv at 3 km to 0.1 ppbv at 19 km [Maiorov et al, 2005]. Pollack et al [1980] suggested SO 2 could be at least partially responsible for the observed absorption at 400-500 nm below the cloud layers, but they did not publish the detailed results of their computations and no subsequent publication has either confirmed or refuted the importance of absorption by SO 2 below 40 km.…”

Section: Sulfur Chemistrymentioning

confidence: 99%