Variations of sulphur dioxide at the cloud top of Venus’s dynamic atmosphere

@article{Marcq2012VariationsOS,
  title={Variations of sulphur dioxide at the cloud top of Venus’s dynamic atmosphere},
  author={Emmanuel Marcq and J L Bertaux and Franck Montmessin and Denis Belyaev},
  journal={Nature Geoscience},
  year={2012},
  volume={6},
  pages={25 - 28}
}
A pulse of sulphur dioxide in Venus’s upper atmosphere was observed by the Pioneer Venus spacecraft in the 1970s and 1980s and attributed to volcanism. Recent sulphur dioxide measurements from Venus Express indicate decadal-scale fluctuations in sulphur dioxide above Venus’s cloud tops in an atmosphere that is more dynamic than expected. Sulphur dioxide is a million times more abundant in the atmosphere of Venus than that of Earth, possibly as a result of volcanism on Venus within the past… Expand

Figures from this paper

Sulfuric acid vapor and sulfur dioxide in the atmosphere of Venus as observed by the Venus Express radio science experiment VeRa
Abstract The Venus Express radio science experiment VeRa provided more than 900 neutral atmospheric profiles between the years 2006 and 2014. About 800 of these could be used for an analysis of theExpand
Sulfur dioxide in the Venus atmosphere: I. Vertical distribution and variability
Abstract Recent observations of sulfur containing species (SO2, SO, OCS, and H2SO4) in Venus’ mesosphere have generated controversy and great interest in the scientific community. These observationsExpand
Distribution of SO 2 content at the night side of Venus' upper mesosphere
Venus has a dense CO 2 atmosphere with a thick cloud layer (50-70 km) consisting of sulfuric acid (H 2 SO 4 ) aerosols. Sulfur oxides (SO x ) are directly associated with those aerosols and plays anExpand
Evidence for SO2 latitudinal variations below the clouds of Venus
Context. Sulphur dioxide (SO2) is highly variable above the clouds of Venus, yet no spatial or temporal variability below the clouds had been known until now. Aims. In order to constrain Venus’sExpand
Sulfur dioxide in the Venus Atmosphere: II. Spatial and temporal variability
The vertical distribution of sulfur species in the Venus atmosphere has been investigated and discussed in Part I of this series of papers dealing with the variability of SO2 on Venus. In this secondExpand
A Recharge Oscillator Model for Interannual Variability in Venus’ Clouds
Sulfur dioxide is a radiatively and chemically important trace gas in the atmosphere of Venus and its abundance at the cloud-tops has been observed to vary on interannual to decadal timescales. ThisExpand
Present-day volcanism on Venus as evidenced from weathering rates of olivine
TLDR
It is shown that olivine becomes coated, within days, with alteration products, primarily hematite (Fe2O3), and the VNIR 1000-nm absorption, characteristic of Olivine, also weakens within days. Expand
Chemically distinct regions of Venus’s atmosphere revealed by measured N2 concentrations
A defining characteristic of the planet Venus is its thick, CO2-dominated atmosphere. Despite over 50 years of robotic exploration of Venus, including thirteen successful atmospheric probes andExpand
Variations of water vapor and cloud top altitude in the Venus’ mesosphere from SPICAV/VEx observations
SPICAV VIS-IR spectrometer on-board the Venus Express mission measured the H 2 O abundance above Venus’ clouds in the 1.38 µm band, and provided an estimation of the cloud top altitude based on CO 2Expand
Night side distribution of SO 2 content in Venus’ upper mesosphere
In this paper we present the first night side distribution of SO 2 content in Venus’ upper mesosphere (altitudes from 85 to 105 km). The dataset is based on the SPICAV UV stellar occultationExpand
...
1
2
3
4
5
...

References

SHOWING 1-10 OF 31 REFERENCES
Sulfur Dioxide: Episodic Injection Shows Evidence for Active Venus Volcanism
TLDR
Pioneer Venus ultraviolet spectra from the first 5 years of operation show a decline in sulfur dioxide abundance at the cloud tops and in the amount of submicron haze above the clouds, implying the episodic injection of sulfur dioxide possibly caused by episodic volcanism. Expand
Sulfur dioxide at the Venus cloud tops, 1978-1986
Ultraviolet spectroscopy from the Pioneer Venus Orbiter shows a decline in the cloud top abundance of SO2 from about 100 ppb to about 10 ppb in the period 1978-1986. A consistent decline in polarExpand
Recent Hotspot Volcanism on Venus from VIRTIS Emissivity Data
TLDR
Variations in the thermal emissivity of the surface observed by the Visible and Infrared Thermal Imaging Spectrometer on the European Space Agency’s Venus Express spacecraft are used to identify compositional differences in lava flows at three hotspots, indicating that Venus is actively resurfacing. Expand
Estimation of the rate of volcanism on Venus from reaction rate measurements
Maintenance of the global H2SO4 clouds on Venus requires volcanism to replenish SO2, which is continually removed from the atmosphere by reaction with calcium minerals on the planet's surface1–4.Expand
An investigation of the SO2 content of the venusian mesosphere using SPICAV-UV in nadir mode
Using the SPICAV-UV spectrometer aboard Venus Express in nadir mode, we were able to derive spectral radiance factors in the middle atmosphere of Venus in the 170-320 nm range at a spectralExpand
Climate control on Venus: Comparison of the carbonate and pyrite models
Abstract We review two models describing the Venus climate system: the carbonate and pyrite models. It has been argued carbonate and pyrite are potentially important minerals controlling the climateExpand
First observations of SO2 above Venus' clouds by means of Solar Occultation in the Infrared
[1] Solar Occultation in the Infrared (SOIR) is a part of the Spectroscopy for Investigation of Characteristics of the Atmosphere of Venus (SPICAV)/SOIR occultation experiment on board Venus ExpressExpand
The composition of the atmosphere of Venus below 100 km altitude: An overview
Abstract We review the progress in our understanding of the composition of the Venus atmosphere since the publication of the COSPAR Venus International Reference Atmosphere volume in 1985. ResultsExpand
A photochemical model for the Venus atmosphere at 47–112 km
Abstract The model is intended to respond to the recent findings in the Venus atmosphere from the Venus Express and ground-based submillimeter and infrared observations. It extends down to 47 km forExpand
Atmospheric Composition, Chemistry, and Clouds
Venus’ atmosphere has a rich chemistry involving interactions among sulfur, chlorine, nitrogen, hydrogen, and oxygen radicals. The chemical regimes in the atmosphere range from ion-neutralExpand
...
1
2
3
4
...