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dc.contributor.authorMikhail, Sami
dc.contributor.authorHeap, Michael J.
dc.date.accessioned2018-05-06T23:33:35Z
dc.date.available2018-05-06T23:33:35Z
dc.date.issued2017-07
dc.identifier.citationMikhail , S & Heap , M J 2017 , ' Hot climate inhibits volcanism on Venus : constraints from rock deformation experiments and argon isotope geochemistry ' , Physics of the Earth and Planetary Interiors , vol. 268 , pp. 18-34 . https://doi.org/10.1016/j.pepi.2017.05.007en
dc.identifier.issn0031-9201
dc.identifier.otherPURE: 249921230
dc.identifier.otherPURE UUID: 0bc652e0-95a4-4170-a088-624ef66fe896
dc.identifier.otherScopus: 85019121733
dc.identifier.otherORCID: /0000-0001-5276-0229/work/37274383
dc.identifier.otherWOS: 000403522500003
dc.identifier.urihttp://hdl.handle.net/10023/13306
dc.descriptionM.J. Heap acknowledges funding from an Initiative d’Excellence (IDEX) “Attractivité” grant (VOLPERM), funded by the University of Strasbourg.en
dc.description.abstractThe disparate evolution of sibling planets Earth and Venus has left them markedly different. Venus’ hot (460 °C) surface is dry and has a hypsometry with a very low standard deviation, whereas Earth’s average temperature is 4 °C and the surface is wet and has a pronounced bimodal hypsometry. Counterintuitively, despite the hot Venusian climate, the rate of intraplate volcano formation is an order of magnitude lower than that of Earth. Here we compile and analyse rock deformation and atmospheric argon isotope data to offer an explanation for the relative contrast in volcanic flux between Earth and Venus. By collating high-temperature, high-pressure rock deformation data for basalt, we provide a failure mechanism map to assess the depth of the brittle–ductile transition (BDT). These data suggest that the Venusian BDT likely exists between 2–12 km depth (for a range of thermal gradients), in stark contrast to the BDT for Earth, which we find to be at a depth of ~25-27 km using the same method. The implications for planetary evolution are twofold. First, downflexing and sagging will result in the sinking of high-elevation structures, due to the low flexural rigidity of the predominantly ductile Venusian crust, offering an explanation for the curious coronae features on the Venusian surface. Second, magma delivery to the surface—the most efficient mechanism for which is flow along fractures (dykes; i.e., brittle deformation)—will be inhibited on Venus. Instead, we infer that magmas must stall and pond in the ductile Venusian crust. If true, a greater proportion of magmatism on Venus should result in intrusion rather than extrusion, relative to Earth. This predicted lower volcanic flux on Venus, relative to Earth, is supported by atmospheric argon isotope data: we argue here that the anomalously unradiogenic present-day atmospheric 40Ar/36Ar ratio for Venus (compared with Earth) must reflect major differences in 40Ar degassing, primarily driven by volcanism. Indeed, these argon data suggest that the volcanic flux on Venus has been three times lower than that on Earth over its 4.56 billion year history. We conclude that Venus’ hot climate inhibits volcanism.
dc.format.extent17
dc.language.isoeng
dc.relation.ispartofPhysics of the Earth and Planetary Interiorsen
dc.rights© 2017 Elsevier B.V. All rights reserved. This work has been made available online in accordance with the publisher’s policies. This is the author created accepted version manuscript following peer review and as such may differ slightly from the final published version. The final published version of this work is available at: https://doi.org/10.1016/j.pepi.2017.05.007en
dc.subjectGE Environmental Sciencesen
dc.subjectQE Geologyen
dc.subjectQB Astronomyen
dc.subjectNDASen
dc.subject.lccGEen
dc.subject.lccQEen
dc.subject.lccQBen
dc.titleHot climate inhibits volcanism on Venus : constraints from rock deformation experiments and argon isotope geochemistryen
dc.typeJournal articleen
dc.description.versionPostprinten
dc.contributor.institutionUniversity of St Andrews.School of Earth & Environmental Sciencesen
dc.contributor.institutionUniversity of St Andrews.St Andrews Centre for Exoplanet Scienceen
dc.contributor.institutionUniversity of St Andrews.St Andrews Isotope Geochemistryen
dc.identifier.doihttps://doi.org/10.1016/j.pepi.2017.05.007
dc.description.statusPeer revieweden
dc.date.embargoedUntil2018-05-06


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