HDO and SO<sub>2</sub>thermal mapping on Venus

Encrenaz, Thérèse; Greathouse, T. K.; Marcq, Emmanuel; Sagawa, Hideo; Widemann, Thomas; Bézard, Bruno; Fouchet, Thierry; Lefèvre, Franck; Lebonnois, Sébastien; Atreya, S. K.; Lee, Yeon Joo; Giles, Rohini; Watanabe, Shigeto; Shao, Wen-Cheng; Zhang, X.; Bierson, C. J.

doi:10.1051/0004-6361/202037741

Cited by 24 publications

(22 citation statements)

References 29 publications

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“…Thus, we would expect sulfur dioxide to vary between one and two orders of magnitude as a result of the convective layer height oscillations. This is in reasonable agreement with the observed magnitude of variability (Encrenaz et al, 2020;Marcq et al, 2013Marcq et al, , 2020. Stronger quantitative arguments would require a more thorough modeling of atmospheric dynamics and chemistry and is a promising direction for future work.…”

Section: Relationship To Observed Sulfur Dioxide Oscillationssupporting

confidence: 85%

A Recharge Oscillator Model for Interannual Variability in Venus’ Clouds

et al. 2020

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The clouds of Venus are among the primary controls of the atmospheric radiative balance, and are composed of sulfuric acid, water and other sulfur-based aerosols which form from the photolysis of sulfur dioxide (Esposito et al., 1983). The main cloud deck can be resolved into three distinct regions, and ranges from 70 to 47 km in the atmosphere (Knollenberg & Hunten, 1980). The upper clouds are formed by the photochemical production of sulfuric acid from sulfur dioxide, the middle clouds by the droplet growth in the convective region, and lower clouds by condensation of sulfuric acid from the lower atmosphere on to the middle cloud droplet flux (Imamura & Hashimoto, 2001; Krasnopolsky & Pollack, 1994; Mills et al., 2007). Climate modeling studies of Venus have noted that the climate state is very sensitive to perturbations of SO 2 , H 2 O and cloud albedo (Bullock & Grinspoon, 2001; Hashimoto & Abe, 2001). Several decades of ground and space based observations of sulfur dioxide show that this trace gas is highly variable at the cloud tops at timescales of hours to decades (

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Section: Relationship To Observed Sulfur Dioxide Oscillationssupporting

confidence: 85%

A Recharge Oscillator Model for Interannual Variability in Venus’ Clouds

et al. 2020

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“…These observations show not only temporal variations of disk-integrated abundances but also a seemingly temporal anticorrelation between SO 2 and H 2 O. The evidence of this anticorrelation is not very clear in Encrenaz et al (2019), but with more data taken recently, the correlation is stronger (Encrenaz et al, 2019b(Encrenaz et al, , 2020. The cause for this anticorrelation is unknown.…”

Section: Introductionmentioning

confidence: 75%

“…In this work we revisited the sulfur-water chemical system in the middle atmosphere of Venus, motivated by the recently and simultaneously observed SO 2 and H 2 O variations at~64 km from TEXES/IRTF (Encrenaz et al, 2019b(Encrenaz et al, , 2020. Using a 1-D chemistry-diffusion model, we studied the coevolution of SO 2 and H 2 O in the middle atmosphere of Venus for the first time.…”

Section: Conclusion and Discussionmentioning

confidence: 99%

“…This explains the SO 2 behavior in Regime II. Encrenaz et al (2019bEncrenaz et al ( , 2020 reported an anticorrelation of disk-averaged abundances of simultaneously observed SO 2 and H 2 O at~64 ± 2 km (near the upper cloud top) in 2012-2019 from TEXES/IRTF. As shown in Figures S5a and 6a, these data provide unique information about how the two parent chemical species vary together in the middle atmosphere.…”

Section: 1029/2019je006195mentioning

confidence: 99%

“…Discriminating these mechanisms requires detailed sulfur-water chemical models and detailed observations in high temporal and spatial resolutions. Encrenaz et al (2019bEncrenaz et al ( , 2020 simultaneously observed variations of SO 2 and H 2 O at 64 km. These observations range from 2012 to 2019 and are made by TEXES in the spectral range around 7.4 μm.…”

Section: Introductionmentioning

confidence: 97%

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Revisiting the Sulfur‐Water Chemical System in the Middle Atmosphere of Venus

et al. 2020

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Sulfur‐water chemistry plays an important role in the middle atmosphere of Venus. Ground‐based observations have found that simultaneously observed SO2 and H2O at ~64 km vary with time and are temporally anticorrelated. To understand these observations, we explore the sulfur‐water chemical system using a one‐dimensional chemistry‐diffusion model. We find that SO2 and H2O mixing ratios above the clouds are highly dependent on mixing ratios of the two species at the middle cloud top (58 km). The behavior of sulfur‐water chemical system can be classified into three regimes, but there is no abrupt transition among these regimes. In particular, there is no bifurcation behavior as previously claimed. We also find that the SO2 self‐shielding effect causes H2O above the clouds to respond to the middle cloud top in a nonmonotonic fashion. Through comparison with observations, we find that mixing ratio variations at the middle cloud top can explain the observed variability of SO2 and H2O. The sulfur‐water chemistry in the middle atmosphere is responsible for the H2O‐SO2 anticorrelation at 64 km. Eddy transport change alone cannot explain the variations of both species. These results imply that variations of species abundance in the middle atmosphere are significantly influenced by the lower atmospheric processes. Continued ground‐based measurements of the coevolution of SO2 and H2O above the clouds and new spacecraft missions will be crucial for uncovering the complicated processes underlying the interaction among the lower atmosphere, the clouds, and the middle atmosphere of Venus.

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