Venus Was Wet: A Measurement of the Ratio of Deuterium to Hydrogen

Donahue, T. M.; Hoffman, J. H.; Hodges, R. R.; Watson, Andrew J.

doi:10.1126/science.216.4546.630

Cited by 409 publications

(223 citation statements)

References 12 publications

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“…However, the atmosphere of Venus currently has about 100,000 times less water than the oceans and atmosphere of the Earth and is strongly enriched in deuterium. The measurements on Venus give D/H = 150 ± 30 (Donahue et al 1982;de Bergh et al 2006) and up to 240 ± 25 of the terrestrial value. This suggests that Venus lost most of its water at some time in the past.…”

Section: Greenhouse Effect and Climate Evolutionmentioning

confidence: 99%

Venus Atmospheric Thermal Structure and Radiative Balance

et al. 2018

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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 extreme climate and weather. This chapter attempts to provide a comprehensive but by no means exhaustive review of the results of the atmospheric thermal structure and radiative balance since the earlier works published in Venus and Venus II books from recent spacecraft and Earth based investigations and summarizes the gaps in [1411][1412][1413][1414] 1986). Thus, most of the new information about the atmospheric thermal structure has come from different remote sensing (Earth based and spacecraft) techniques using occultations (solar infrared, stellar ultraviolet and orbiter radio occultations), spectroscopy and microwave, short wave and thermal infrared emissions. The results are restricted to altitudes higher than about 40 km, except for one investigation of the near surface static stability inferred by Meadows and Crisp (J. Geophys. Res. 101:4595-4622, 1996) from 1 μm observations from Earth. Little information about the lower atmospheric structure is possible below about 40 km altitude from radio occultations due to large bending angles. The gaps in our knowledge include spectral albedo variations over time, vertical variation of the bulk composition of the atmosphere (mean molecular weight), the identity, properties and abundances of absorbers of incident solar radiation in the clouds. The causes of opacity variations in the nightside cloud cover and vertical gradients in the deep atmosphere bulk composition and its impact on static stability are also in need of critical studies. The knowledge gaps and questions about Venus and its atmosphere provide the incentive for obtaining the necessary measurements to understand the planet, which can provide some clues to learn about terrestrial exoplanets.

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Section: Greenhouse Effect and Climate Evolutionmentioning

confidence: 99%

Venus Atmospheric Thermal Structure and Radiative Balance

et al. 2018

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“…Evidence that the atmosphere of Venus has lost most of its water (assuming it had acquired a large quantity) came from the Pioneer Venus measurements of the d/h ratio, which is about 100 times the terrestrial value [McElroy et al, 1982;Donahue et al, 1982] and has been confirmed by Earthbased spectroscopy [de Bergh et al, 1991]. This implies that Venus has likely lost at least the equivalent of 100 times more water than its present reservoir.…”

Section: Atmospheric Chemistry and Atmospheric Evolutionmentioning

confidence: 93%

Atmospheric composition, chemistry, and clouds

Mills¹,

Esposito²,

Yung³

2007

Geophysical Monograph Series

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“…Two results were of particular importance to geology. One was the discovery by one of the probes of the so-called deuterium anomaly, a D/H ratio larger by a factor of 150 than it is in Earth's oceans [Donahue et al, 1982]. This implies significant hydrogen escape from the planet, suggesting that early in its history Venus could have lost a large amount of water [e.g., Donahue and Russel, 1997].…”

Section: History Of Venus Explorationmentioning

confidence: 99%

Surface evolution of Venus

Basilevsky

McGill

2007

Geophysical Monograph Series

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This chapter contains short descriptions of material units and structures observed on the surface of Venus as well as an abbreviated history of discoveries, that led to the current knowledge of this planet's geology. It is shown that observed units and structures are broadly similar and commonly exhibit similar age sequences in different regions of the planet, although there is debate as to what degree these sequences can be integrated into any single global stratigraphic model. There is a broad consensus concerning the recent general geodynamic style of Venus (no plate tectonics), on the dominating role of basaltic volcanism in the observed crust-forming processes, and on the significant roles of both compressional and extensional tectonic deformation. Also not under debate is that we see the morphologic record of only the last ~1 b.y. (or less) of the history of this planet and that during this time period the role of exogenic resurfacing was very minor. Several important unresolved questions of Venus geology are formulated and suggestions for future missions, that could lead to resolving them are given.

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Venus Was Wet: A Measurement of the Ratio of Deuterium to Hydrogen

Cited by 409 publications

References 12 publications

Venus Atmospheric Thermal Structure and Radiative Balance

Venus Atmospheric Thermal Structure and Radiative Balance

Atmospheric composition, chemistry, and clouds

Surface evolution of Venus

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