Hot climate inhibits volcanism on Venus: Constraints from rock deformation experiments and argon isotope geochemistry

Citation data:

Physics of the Earth and Planetary Interiors, ISSN: 0031-9201, Vol: 268, Page: 18-34

Publication Year:
2017
Usage 2
Abstract Views 2
Captures 4
Readers 4
Mentions 3
News Mentions 3
Social Media 62
Tweets 35
Shares, Likes & Comments 27
DOI:
10.1016/j.pepi.2017.05.007
Author(s):
Sami Mikhail, Michael J. Heap
Publisher(s):
Elsevier BV
Tags:
Physics and Astronomy, Earth and Planetary Sciences
Most Recent Tweet View All Tweets
Most Recent News Mention
article description
The 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 and 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-relief 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 40 Ar/ 36 Ar ratio for Venus (compared with Earth) must reflect major differences in 40 Ar 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.

This article has 0 Wikipedia mention.