Stratigraphic and geographic distribution of steep‐sided domes on Venus: Preliminary results from regional geological mapping and implications for their origin

Иванов, М. А.; Head, J. W.

doi:10.1029/1999je001039

Cited by 28 publications

(23 citation statements)

References 35 publications

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“…highly siliceous: Pavri et al 1992;Petford 2000) or even the melting of basaltic crust (e.g. Ivanov & Head 1999), although these possibilities of tholi formation cannot be ruled out, especially if a tholus did not form in association with a corona (Ivanov & Head 1999, 2004 and/or melting of more felsic crustal material occurred. Instead, the presence of steepsided domes that occur at coronae could be explained as mafic crystal mushes or even highly vesiculated mafic magma (e.g.…”

Section: Evolutionary Modelmentioning

confidence: 97%

“…Consequently, the tholi do not have to represent highly evolved felsic compositions nor do they also need to represent the melting of basaltic crust (e.g. Ivanov & Head 1999) owing to the fact that the heat needed to melt the crust probably went away with the dissipation of mantle upwelling. Ultimately, the timing of the erupted products with corona collapse suggests an intimate connection between the two processes, and any model that explains the volcanic evolution of these three coronae must take this into account.…”

Section: Coronae Analysismentioning

confidence: 99%

“…Tholi have also been noted to occur with some coronae where they typically occur on the annulus (Pavri et al 1992), suggesting that they reflect some of the latest stages of corona-related volcanism. Tholi have also been predicted to form from either differentiation of basaltic magma to produce silicic magmas (Pavri et al 1992;Ivanov & Head 1999;Petford 2000; see also McKenzie et al 1992;Fink et al 1993), the melting of basaltic crust to produce more silica-rich magmas (Ivanov & Head 1999) or the eruption of a high-viscosity basaltic foam due to volatile enhancement in the upper part of the magma reservoir (Pavri et al 1992; see also Stofan et al 2000). Clearly, volcanism has played a fundamental role in corona development where the style and volume of volcanism may be largely dictated by magma supply rates related to the corona (e.g.…”

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confidence: 99%

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The magmatic evolution of three Venusian coronae

Lang

López

2013

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The volcanic and tectonic histories of Venusian coronae appear to be intricately linked. We explore that link through the construction of geological maps of three coronae using Magellan synthetic aperture radar (SAR) imagery and altimetry radar data. Each examined corona -Aramaiti, Bhumidevi and Zemire Coronae -is characterized by an annulus of concentric fractures, lava flows, tholi and clusters of small shields. Radial fractures occur at one corona (Bhumidevi Corona), whereas the other two coronae (Aramaiti and Zemire Coronae) occur within linear fracture belts. Based on observed timing relationships, we propose that the evolution of these three coronae is similar to large silicic caldera formation on Earth in that the formation of concentric fractures facilitated a mass evacuation of a magma reservoir residing underneath each corona resulting in subsequent corona collapse. Our model emphasizes the late-stage evolution of these coronae and predicts that all the erupted products could be basaltic. Such predictions are testable through continued geological mapping of coronae, as well as through in situ spectral analyses by Venusian landers.

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Section: Evolutionary Modelmentioning

confidence: 97%

Section: Coronae Analysismentioning

confidence: 99%

mentioning

confidence: 99%

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The magmatic evolution of three Venusian coronae

Lang

López

2013

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“…In a global study of the stratigraphy and distribution of these volcanic types, Ivanov and Head (1999) found that these volcanic morphologies are "old" features in the evolution of the volcanic plains. , that is, composite units formed by volcanic materials that cannot be differentiated due to homogenization processes (Arvidson et al, 1992) and/or lack of clear primary structures (e.g.…”

Section: [Figure 1]mentioning

confidence: 99%

Embayed intermediate volcanoes on Venus: Implications for the evolution of the volcanic plains

López

2011

Icarus

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“…Furthermore, larger features typical of volcanism on Mars [such as huge volcanic edifices and calderas (Carr 1973;Crumpler et al 1996)], and not seen on the Moon (Head and Wilson 1991), were not observed by Mariner 10 on Mercury. Also not observed in the Mariner 10 data were examples of the large (10-30 km diameter) steep-sided domes suggestive of crustal magmatic differentiation processes seen on the Moon (Head and McCord 1978;Chevrel et al 1999) and Venus (Pavri et al 1992;Ivanov and Head 1999). Lobate fronts exposed at the edge of smooth plains occurrences on Mercury ( Fig.…”

Section: Geological Processes On Mercury: Volcanism and Plains Formationmentioning

confidence: 99%

The Geology of Mercury: The View Prior to the MESSENGER Mission

Head¹,

Chapman²,

Domingue³

et al. 2007

The Messenger Mission to Mercury

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Mariner 10 and Earth-based observations have revealed Mercury, the innermost of the terrestrial planetary bodies, to be an exciting laboratory for the study of Solar System geological processes. Mercury is characterized by a lunar-like surface, a global magnetic field, and an interior dominated by an iron core having a radius at least three-quarters of the radius of the planet. The 45% of the surface imaged by Mariner 10 reveals some distinctive differences from the Moon, however, with major contractional fault scarps and huge expanses of moderate-albedo Cayley-like smooth plains of uncertain origin. Our current image coverage of Mercury is comparable to that of telescopic photographs of the Earth's Moon prior to the launch of Sputnik in 1957. We have no photographic images of one-half of the surface, the resolution of the images we do have is generally poor (∼1 km), and as with many lunar telescopic photographs, much of the available surface of Mercury is distorted by foreshortening due to viewing geometry, or poorly suited for geological analysis and impact-crater counting for age determinations because of high-Sun illumination conditions. Currently available topographic information is also very limited. Nonetheless, Mercury is a geological laboratory that represents (1) a planet where the presence of a huge iron core may be due to impact stripping of the crust and upper mantle, or alternatively, where formation of a huge core may have resulted in a residual mantle and crust of potentially unusual composition and structure; (2) a planet with an internal chemical and mechanical structure that provides new insights into planetary thermal history and the relative roles of conduction and convection in planetary heat loss; (3) a one-tectonic-plate planet where constraints on major interior processes can be deduced from the geology of the global tectonic system; (4) a planet where volcanic resurfacing may not have played a significant role in planetary history and internally generated volcanic resurfacing may have ceased at ∼3.8 Ga; (5) a planet where impact craters can be used to disentangle the fundamental roles of gravity and mean impactor velocity in determining impact crater morphology and morphometry; (6) an environment where global impact crater counts can test fundamental concepts of the distribution of impactor populations in space and time; (7) an extreme environment in which highly radar-reflective polar deposits, much more extensive than those on the Moon, can be better understood; (8) an extreme environment in which the basic processes of space weathering can be further deduced; and (9) a potential end-member in terrestrial planetary body geological evolution in which the relationships of internal and surface evolution can be clearly assessed from both a tectonic and volcanic point of view. In the half-century since the launch of Sputnik, more than 30 spacecraft have been sent to the Moon, yet only now is a second spacecraft en route to Mercury. The MESSENGER mission will address key questions ...

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Stratigraphic and geographic distribution of steep‐sided domes on Venus: Preliminary results from regional geological mapping and implications for their origin

Cited by 28 publications

References 35 publications

The magmatic evolution of three Venusian coronae

The magmatic evolution of three Venusian coronae

Embayed intermediate volcanoes on Venus: Implications for the evolution of the volcanic plains

The Geology of Mercury: The View Prior to the MESSENGER Mission

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