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

  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},
  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… 

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 an

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’s

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. This

Present-day volcanism on Venus as evidenced from weathering rates of olivine

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.

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 and

Venus Atmospheric Thermal Structure and Radiative Balance

From the discovery that Venus has an atmosphere during the 1761 transit by M. Lomonosov to the current exploration of the planet by the Akatsuki orbiter, we continue to learn about the planet’s



Sulfur Dioxide: Episodic Injection Shows Evidence for Active Venus Volcanism

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.

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 polar

Recent Hotspot Volcanism on Venus from VIRTIS Emissivity Data

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.

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.

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 Express

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-neutral