The science goals of the EnVision Venus orbiter mission

Ghail, R. C.; Wilson, Colin; Widemann, Thomas; Titov, Dmitrij; Ansan, V.; Bovolo, Francesca; Breuer, D.; Bruzzone, Lorenzo; Campbell, B. A.; Dumoulin, Caroline; Helbert, Jörn; Hensley, S.; Kiefer, W. S.; Komatsu, G.; Gall, Alice Le; Marcq, Emmanuel; Mason, Philippa J.; Robert, Séverine; Rosenblatt, P.; Vandaele, Ana Carine

doi:10.5194/epsc2020-599

Cited by 17 publications

(17 citation statements)

References 1 publication

Supporting

Mentioning

Contrasting

Order By: Relevance

“…A long‐term baseline analysis will be possible in near the future with the proposed ESA mission Envision. The radio science measurements would obtain convective layer height information, and the VenSpec suite of spectrographic instruments intends to observe water and sulfur dioxide above and below the clouds (Ghail et al., 2017). In addition to the data from the previous missions, these high‐resolution measurements will have a sufficiently long time baseline capable of determining the existence and dominant periods of such oscillations.…”

Section: Resultsmentioning

confidence: 99%

A Recharge Oscillator Model for Interannual Variability in Venus’ Clouds

et al. 2020

View full text Add to dashboard Cite

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 (

show abstract

Section: Resultsmentioning

confidence: 99%

A Recharge Oscillator Model for Interannual Variability in Venus’ Clouds

et al. 2020

View full text Add to dashboard Cite

show abstract

“…Future missions will indubitably provide important clues about present-day activities on the planet (e.g., Glaze et al, 2018). NASA's Venus Emissivity, Radio Science, InSAR, Topography & Spectroscopy mission (Smrekar et al, 2020) and ESA's EnVision mission (Ghail et al, 2012(Ghail et al, , 2020 will return complementary, critical datasets including improved topography, SAR imaging, gravity, and infrared spectroscopy. Additionally, NASA's Deep Atmosphere Venus Investigation of Noble gases, Chemistry, and Imaging mission (Garvin et al, 2022) will analyze gases typically extruded by active volcanoes (SO 2 , CO 2 , HCL, HF, and perhaps PH 3 ).…”

Section: Discussionmentioning

confidence: 99%

Extended Rift‐Associated Volcanism in Ganis Chasma, Venus Detected From Magellan Radar Emissivity

Brossier

Gilmore

Head

2022

Geophysical Research Letters

View full text Add to dashboard Cite

The diameter of Venus predicts that it should, like Earth, be volcanically active today (e.g., Head & Solomon, 1981). Radar images of the surface collected during the Magellan mission (1990)(1991)(1992)(1993)(1994) did not identify any morphological evidence of recent volcanic activity. Nonetheless, recent and ongoing volcanic activity on Venus is suggested by other multiple independent lines of evidence. Pioneer Venus Orbiter (PV, 1978(PV, -1986 and Venus Express (VEx, 2005(VEx, -2014 missions gathered more than 30 years of atmospheric measurements searching for evidence of possible volcanic eruptions. Both missions revealed fluctuations in sulfur dioxide (SO 2 ) that are possibly associated with volcanic outgassing on Venus (

show abstract

“…The methodology used could provide a significant contribution to the key debate regarding the style of resurfacing on Venus. Their results demonstrate what can be still achieved using the (relatively low resolution) Magellan radar data set but it also shows what could be potentially obtained by higher resolution radar data which are going to be provided from future missions to Venus, such as the European Space Agency's EnVision mission (Ghail et al, 2012(Ghail et al, , 2020 or the NASA's Venus Emissivity, Radio Science, InSAR, Topography & Spectroscopy mission (i.e., Smrekar et al, 2020). The Deep Atmosphere of Venus Investigation of Noble gases, Chemistry and Imaging, Plus (DAVINCI+) (Garvin et al, 2020;Glaze et al, 2017Glaze et al, , 2018 and Venera-D (Senske et al, 2017;Zasova et al, 2019) missions will instead provide more detailed data on the structure and thermal profiles of the Venusian atmosphere.…”

mentioning

confidence: 85%