Geologic units on Venus: evidence for their global correlation

Basilevsky, A. T.; Head, J. W.

doi:10.1016/s0032-0633(99)00083-5

Cited by 94 publications

(145 citation statements)

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“…Grosfils & Head 1996, Nagasawa et al 1998 and will also help establish the relationship(s) between the dike swarms, their volcano-tectonic centers, and both regional and broader scale stratigraphie sequences developed by other authors (e.g. Ivanov & Head 1996;Basilevsky & Head 1998, 2000bCopp et al 1998;Guest & Stofan 1999;DeShon et al 2000;Hansen 2000).…”

Section: Outstanding Issuesmentioning

confidence: 90%

Giant Dike Swarms: Earth, Venus, and Mars

Ernst

Grosfils

Mège

2001

Annu. Rev. Earth Planet. Sci.

300

137

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▪ Abstract Earth, Venus, and Mars all exhibit populations of giant (radiating, linear, and arcuate) mafic dike swarms hundreds to >2000 km in length. On Earth the dikes are exposed by erosion, while on Venus and Mars their presence is mainly inferred from associated volcanic morphology and surface deformation. The apparent absence of plate tectonics in the geologic record of Venus and Mars means that the observed population of swarms remains geometrically intact, while on Earth plate tectonics has fragmented swarms. About 30 giant radiating swarms have so far been identified on Earth, but with further study the number is expected to rise and may eventually coincide with the hundreds of mantle plume head events now being proposed. On Venus, at least 118 radiating swarms are distributed across the planet, and new high resolution mapping is revealing additional swarms. On Mars, up to 16 giant dike swarms are observed, most associated with the Tharsis region.

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Section: Outstanding Issuesmentioning

confidence: 90%

Giant Dike Swarms: Earth, Venus, and Mars

Ernst

Grosfils

Mège

2001

Annu. Rev. Earth Planet. Sci.

300

137

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“…Many researchers prefer to call the first one "Ridged plains" [e.g., Bridges and McGill, 2002;Campbell and Campbell, 2002] or "Regional plains" [e.g., Brian et al, 2005;McGill, 2000] as we do here. Regional plains occupy 50-60% of the surface [Basilevsky and Head, 2000a]. They have a rather smooth (at the scale of observation) surface (Figure 7), often with flow-like features, which are inferred to be solidified lava flows [Guest et al, 1992;Head et al, 1992].…”

Section: Current View Of Surface Features and Unitsmentioning

confidence: 99%

“…A terrain of this type is also observed in many coronae (see below), where radial and concentric structural patterns of dense fracturing are typical. Global abundance of outcrops of the densely fractured plains material is about 3 to 5% [Basilevsky and Head, 2000a].…”

Section: Current View Of Surface Features and Unitsmentioning

confidence: 99%

“…In most observed cases, regional plains embay the belts [e.g., Head, 1998, 2000;Bridges and McGill, 2002;Ivanov and Head, 2004a] although in some places their age relations are ambiguous [e.g., Rosenberg and McGill, 2001]. Global abundance of ridge belts is about 3 to 5% [Basilevsky and Head, 2000a].…”

Section: Current View Of Surface Features and Unitsmentioning

confidence: 99%

“…Most likely the main reason for this disagreement stems from different criteria used for these studies, and different areas of shield plains sampled. Global abundance of shield plains was estimated by Basilevsky and Head [2000a] as close to 10-15%.…”

Section: Current View Of Surface Features and Unitsmentioning

confidence: 99%

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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: Interpreting the spatial distribution of volcanically modified craters

O’Rourke

Wolf

Ehlmann

2014

Geophysical Research Letters

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To understand the impact cratering record on Venus, we investigate two distinct resurfacing styles: localized, thin flows and large shield volcanoes. We statistically analyze the size-frequency distribution of volcanically modified craters and, using Monte Carlo simulations, their spatial distribution. Lava flows partially fill most craters, darkening their floors in radar images. We find that a model featuring localized, thin flows occurring throughout geologic time predicts their observed distribution. Individual flows may be morphologically indistinguishable, but, combined, they cover large provinces. Recent mantle plumes may drive a small amount of hot spot magmatism that produces the observed clusters of large shield volcanoes and obviously embayed craters. Ultimately, our analysis demonstrates that two styles of volcanism are needed to explain the observed properties of impact craters and that catastrophic resurfacing is not required.

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Geologic units on Venus: evidence for their global correlation

Cited by 94 publications

References 81 publications

Giant Dike Swarms: Earth, Venus, and Mars

Giant Dike Swarms: Earth, Venus, and Mars

Surface evolution of Venus

Venus: Interpreting the spatial distribution of volcanically modified craters

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