2016
DOI: 10.1002/2015ja022226
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Solar XUV and ENA‐driven water loss from early Venus' steam atmosphere

Abstract: We present a study on the influence of the upper atmosphere hydrodynamic escape of hydrogen, driven by the solar soft X‐ray and extreme ultraviolet radiation (XUV), on an expected outgassed steam atmosphere of early Venus. By assuming that the young Sun was either a weak or moderately active young G star, we estimated the water loss from a hydrogen dominated thermosphere due to the absorption of the solar XUV flux and the precipitation of solar wind produced energetic hydrogen atoms (ENAs). The production of E… Show more

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Cited by 40 publications
(55 citation statements)
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“…This would be accomplished by sequestering the O 2 left behind by H 2 O dissociation in the magmatic crust and upper mantle (e.g. Lebrun et al, 2013;Gillmann et al, 2009;Lichtenegger et al, 2016;Lammer et al, 2018). We discuss how large quantities of O 2 can be lost after a significant period of habitability in bullet 6 of Section 8, in lieu of early MO losses.…”
Section: Venus' Early Evolution and Evidence For Watermentioning
confidence: 99%
See 2 more Smart Citations
“…This would be accomplished by sequestering the O 2 left behind by H 2 O dissociation in the magmatic crust and upper mantle (e.g. Lebrun et al, 2013;Gillmann et al, 2009;Lichtenegger et al, 2016;Lammer et al, 2018). We discuss how large quantities of O 2 can be lost after a significant period of habitability in bullet 6 of Section 8, in lieu of early MO losses.…”
Section: Venus' Early Evolution and Evidence For Watermentioning
confidence: 99%
“…The timing of the MO termination is critical in more than one way. If the steam and CO 2 atmosphere cooled sufficiently for MO crystallization to occur by the time of the Late Veneer (also referred to as "Late Accretion") then even if Venus lost most/all of its primordial H 2 O through escape processes (Gillmann et al, 2009;Hamano et al, 2013;Lichtenegger et al, 2016) there may have been a second chance to obtain a surface ocean, albeit a shallow one. Recent work by Greenwood et al (2018) implies that Earth may have received as much as 30% of its H 2 O inventory in post-accretion impact delivery, consistent with research that shows that the entire H 2 O budget cannot come from the late veneer (Morbidelli & Wood, 2015).…”
Section: Venus' Early Evolution and Evidence For Watermentioning
confidence: 99%
See 1 more Smart Citation
“…However, more recent models of the winds of young Sun-like stars (Johnstone et al, 2015a) suggests that they were much more tenuous than previously expected. The resulting energy input into planetary atmospheres by production of energetic neutral atoms is thus not very efficient and the stellar EUV luminosity is the dominant driver of atmospheric escape (Lichtenegger et al, 2016).…”
Section: Euv Evolution and Wind Of The Young Sunmentioning
confidence: 99%
“…If the young host star's EUV flux is not too high, some residual O 2 may remain in the atmosphere as a product of H 2 O dissociation, while the hydrogen atoms escape hydrodynamically (Zahnle and Kasting, 1986). The remaining oxygen and atmospheric nitrogen could have been incorporated into the planet's hot magmatic crust, where they oxidized the upper mantle (Gillmann et al, 2009;Hamano et al, 2013;Kurosawa, 2015;Lichtenegger et al, 2016;Wordsworth, 2016;Lammer et al, 2018). Under such conditions, the highly oxidized surface material can be mixed with reduced, nitrogen-rich material.…”
Section: Hypothetical Scenarios For the Evolution Of N 2 Atmospheresmentioning
confidence: 99%