Coronae on Venus: Morphology, classification, and distribution

Pronin, A. A.; Stofan, E. R.

doi:10.1016/0019-1035(90)90148-3

Cited by 86 publications

(56 citation statements)

References 15 publications

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“…And between the coronae and the domal uplifts (such as Beta Regio)? • What are the reasons for the differences in size and complexity (Pronin and Stofan, 1990) between coronae? Why do the more evolved larger coronae (Rananeida, for instance) seem to have finished their evolution earlier?…”

Section: Discussionmentioning

confidence: 99%

Ovoid structures in the solar system: The coronae of Venus and Miranda, and the domes on the Earth

Anguita

Chicarro

1991

Earth Moon Planet

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Section: Discussionmentioning

confidence: 99%

Ovoid structures in the solar system: The coronae of Venus and Miranda, and the domes on the Earth

Anguita

Chicarro

1991

Earth Moon Planet

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“…On the basis of stratigraphic relations, tessera is generally considered to be the oldest surface exposed on Venus. Coronae are circular features characterized by concentric and, in some cases, radial, tectonic lineations (Barsukov and others, 1986;Pronin and Stofan, 1990). Topographically, coronae include domes, plateaus, plateaus with interior lows, or rimmed depressions (Stofan and others, 1992).…”

Section: General Geologymentioning

confidence: 99%

Geologic map of the Carson Quadrangle (V-43), Venus

Bender¹,

Senske²,

Greeley³

2000

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“…Ovoids and coronae (Stofan and Head, 1990;Pronin and Stofan, 1990) have several characteristics in common and are discussed in more detail in subsequent sections. Craters of apparent impact origin have been mapped in this area ( Figure 2c) (Table II) are distributed relatively evenly across the surface Campbell et al, 1991) despite some clustering, typically in the lowlands (southern Guinevere Planitia, southern Navka Planitia), with the upland containing Ushas, Innini and Hathor Montes, Themis Regio and Alpha Regio showing slightly lower concentrations.…”

Section: Structures Cratersmentioning

confidence: 99%

Geology and tectonics of the Themis Regio-Lavinia Planitia-Alpha Regio-Lada Terra area, Venus: Results from Arecibo image data

et al. 1991

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New radar images obtained from the Arecibo Observatory (resolution 1.5-4.0km) for portions of the southern hemisphere of Venus show that: the upland of Phoebe Regio contains the southern extension of Devana Chasma, a rift zone extending 4200 km south from Theia Mons and interpreted as a zone of extension; Alpha Regio, the only large region of tessera within the imaged area; is similar to tessera mapped elsewhere on the planet and covers a smaller percentage of the surface than that observed in the northern high latitudes; the upland made of Ushas, Innini and Hathor Montes consists of three distinct volcanic constructs; Themis Regio is mapped as an ovoid chain of radar-bright arcuate single and double ring structures, edifices and bright lineaments. This area is interpreted as a region of mantle upwelling and on the basis of apparent split and separated features, a zone of localized faulting and extension. Linear zones of deformation in Lavinia Planitia are characterized by lineament belts that are often locally elevated, are similar to ridge belts mapped in the northern high latitudes and are interpreted to be characterized mainly by compression; radar-bright lava complexes within Lavinia Planitia are unique to this part of the planet and are interpreted to represent areas of eruption of high volumes of extremely fluid lava; the upland of Lada Terra is bound to the north by a linear deformation zone interpreted as extensional, is characterized by large ovoids and coronae, is interpreted to be associated with an area of mantle upwelling, and is in contrast to the northern high latitude highland of Ishtar Terra. Regions of plains in the southern hemisphere cover about 78% of the mapped area and are interpreted to be volcanic in origin. Located within the area imaged (10-78" S) are 52 craters interpreted to be of impact origin ranging from 8 to 157 km in diameter. On the basis of an overall crater density of 0.94 craters/lo6 km', it is determined that the age of this part of the Venus surface is similar to the 0.3 to 1.0 billion year age calculated for the equatorial region and northern high latitudes. The geologic characteristics of the portion of the Venus southern hemisphere imaged by Arecibo are generally similar to those mapped elsewhere on the planet. This part of the planet is characterized by widespread volcanic plains, large volcanic edifices, and zones of linear belt deformation. The southern hemisphere of Venus differs from northern high latitudes in that tessera makes up only a small percentage of the surface area and the ovoid chain in Themis Regio is unique to this part of the planet. On the basis of the analysis presented here, the southern hemisphere of Venus is interpreted to be characterized by regions of mantle upwelling on a variety of scales (ovoids, region made up of Ushas, Innini and Hathor Montes), upwelling and extension (Themis Regio) and localized compression (lineament belts in Lavinia Planitia).

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Coronae on Venus: Morphology, classification, and distribution

Cited by 86 publications

References 15 publications

Ovoid structures in the solar system: The coronae of Venus and Miranda, and the domes on the Earth

Ovoid structures in the solar system: The coronae of Venus and Miranda, and the domes on the Earth

Geologic map of the Carson Quadrangle (V-43), Venus

Geology and tectonics of the Themis Regio-Lavinia Planitia-Alpha Regio-Lada Terra area, Venus: Results from Arecibo image data

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