The VenSpec suite on the ESA EnVision mission to Venus

Helbert, J.; Vandaele, Ann Carine; Marcq, Emmanuel; Robert, Séverine; Ryan, Conor; Guignan, Gabriel; Rosas-Ortiz, Yaquelin M.; Neefs, Eddy; Thomas, Ian; Arnold, Gabriele; Peter, G.; Widemann, Thomas; Lara, L. M.

doi:10.1117/12.2529248

Cited by 22 publications

(19 citation statements)

References 8 publications

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“…Large volcanic rises like Atla Regio represent one important science target for future orbital and in‐situ investigations as they are possible sites of current tectonic and volcanic activity. The proposed missions VERITAS (NASA); (Helbert et al., 2018; Hensley et al., 2020; Smrekar et al., 2020) and EnVision (ESA) (Ghail et al., 2018; Helbert et al., 2019) would return complementary, critical datasets including improved topography, SAR imaging, gravity, and infrared spectroscopy. Such data are essential to better map the radar properties, distribution, sources and stratigraphy of the lava flows at Atla Regio and place in context with improved gravity and new measurements of infrared emissivity which will constrain rock composition, thermal anomalies and atmospheric composition and variability.…”

Section: Discussionmentioning

confidence: 99%

Distinct Mineralogy and Age of Individual Lava Flows in Atla Regio, Venus Derived From Magellan Radar Emissivity

et al. 2021

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Previous studies of NASA's Magellan radar data showed that most of the Venus highlands exhibit a single reduction in radar emissivity values at high altitudes, above 6,053 km (Klose et al., 1992; Pettengill et al., 1992). This decline in radar emissivity with altitude is ascribed to the presence of minerals with a high dielectric constant produced by chemical weathering reactions between the rocks and the near-surface atmosphere. It is expected from theory that materials with high dielectric constants will enhance their radar reflectivity and lower their radar emissivity (Campbell, 1994; Pettengill et al., 1992). Proposed minerals include: (1) pyrite produced through sulfidation and/or oxidation of iron (

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Section: Discussionmentioning

confidence: 99%

Distinct Mineralogy and Age of Individual Lava Flows in Atla Regio, Venus Derived From Magellan Radar Emissivity

et al. 2021

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“…Ground-and space-based observations in near-infrared window regions permit remote sounding of a few major gases, but many minor species which may play important catalytic or intermediate roles in chemical cycles are difficult or impossible to probe remotely. Mapping spatial variation of volcanically gases could be a direct way of finding active volcanism on Venus; this can be achieved using spectroscopy in nightside near-infrared, as is being developed for the EnVision M5 mission [30]. Further to this, measurement from a descent probe of near surface chemical abundances and their vertical profiles will permit determination of whether there are active surface-atmosphere exchanges taking place and of what surface reactions are buffering the atmospheric composition.…”

Section: Chemistry and Cloudsmentioning

confidence: 99%

Venus: key to understanding the evolution of terrestrial planets

2021

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In this paper, originally submitted in answer to ESA’s “Voyage 2050” call to shape the agency’s space science missions in the 2035–2050 timeframe, we emphasize the importance of a Venus exploration programme for the wider goal of understanding the diversity and evolution of habitable planets. Comparing the interior, surface, and atmosphere evolution of Earth, Mars, and Venus is essential to understanding what processes determined habitability of our own planet and Earth-like planets everywhere. This is particularly true in an era where we expect thousands, and then millions, of terrestrial exoplanets to be discovered. Earth and Mars have already dedicated exploration programmes, but our understanding of Venus, particularly of its geology and its history, lags behind. Multiple exploration vehicles will be needed to characterize Venus’ richly varied interior, surface, atmosphere and magnetosphere environments. Between now and 2050 we recommend that ESA launch at least two M-class missions to Venus (in order of priority): a geophysics-focussed orbiter (the currently proposed M5 EnVision orbiter – [1] – or equivalent); and an in situ atmospheric mission (such as the M3 EVE balloon mission – [2]). An in situ and orbital mission could be combined in a single L-class mission, as was argued in responses to the call for L2/L3 themes [3–5]. After these two missions, further priorities include a surface lander demonstrating the high-temperature technologies needed for extended surface missions; and/or a further orbiter with follow-up high-resolution surface radar imaging, and atmospheric and/or ionospheric investigations.

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Section: Introductionmentioning

confidence: 99%

“…In response to these successes, the Venus Emissivity Mapper (VEM) concept was developed for future orbital missions to enable Venus' surface to be studied from orbit through six different windows at 0.86, 0.91, 0.99, 1.02, 1.11, and 1.18 µm (Helbert et al, 2018(Helbert et al, , 2019. It is proposed as part of the VERITAS (Helbert et al, 2018;Smrekar et al, 2020) and Envision (Helbert et al, 2019) missions. In a manner analogous to the eight-filter imaging on the Pancam instrument of the Mars Exploration rovers (Bell et al, 2003) or the imaging of the surface of Titan by the VIMS instrument on the Cassini mission (Barnes et al, 2007), the six windows can provide a wealth of information on surface composition.…”

Section: Introductionmentioning

confidence: 99%