Corona Classification by Evolutionary Stage

DeLaughter, John; Jurdy, Donna M.

doi:10.1006/icar.1999.6087

Cited by 27 publications

(17 citation statements)

References 30 publications

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“…Significant numbers (52) of polygon fields are associated with coronae and coronae‐like features (see Figures 12 and 13). Of these, approximately half of the locations contain previously identified coronae [ DeLaughter and Jurdy , 1999; Stofan et al , 2001], including three type 2 coronae with partial fracture annuli [ Stofan et al , 2001]. Some features that we identify as coronae are less than 50 km in diameter and were probably overlooked in other surveys.…”

Section: Relationship To Other Geologic Featuresmentioning

confidence: 81%

Characterization and formation of polygonal fractures on Venus

2002

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[1] Fracture theory predicts that polygonal cracks will form in the presence of an isotropic, extensional stress field. On Venus, polygonal fractures are observed on scales several orders of magnitude larger than on Earth, with an average diameter of 1.8 ± 0.9 km. Proposed formation mechanisms include cooling following lava flow emplacement, lithospheric heating, and climate change. Here we examine the characteristics and geologic setting of 204 regions of polygons. Some regions display two spatially overlapping size ranges, with the larger spacing typically 10-25 km. Most polygonal fractures appear to be extensional, but some have the morphology of compressional ridges. Polygons are confined to plains regions and occur in association with shield fields (49%), coronae and coronae-like features (21.3%), tessera (17.5%), and wrinkle ridges (20%). In locations where polygons occur with shield fields, coronae, or both, they appear to have formed contemporaneously. Formation in conjunction with local heating events is consistent with the lithospheric cooling hypothesis. However, there is almost never the predicted decrease in size away from the center of coronae or shield fields. Only a small percentage of coronae and shield fields contain polygons, indicating that they are not typical of the formation process. The climate change-induced scenario is consistent with many characteristics of the polygons, including the small and large size ranges, the compressional ridges, and their occurrence with and without evidence of local heating. Although polygons may have diverse origins, including formation by multiple deformation events, overall polygon characteristics support the climate change hypothesis.

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Section: Relationship To Other Geologic Featuresmentioning

confidence: 81%

Characterization and formation of polygonal fractures on Venus

2002

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“…Recent finite-element modelling indicates that radial fractures form during early mantle diapir impingement, with an outward propagation of dykes occurring at a later stage due to loadinginduced downward lithospheric flexure ). Together with novae, then, coronae with a topographically positive central dome and radial fracture system may represent the first stage of mantle plume upwelling, and coronae with a central annular depression might be typical of the final stage DeLaughter & Jurdy 1999). In another analysis, however, Gerya (2014) proposed a variation of this general process.…”

Section: Volcanismmentioning

confidence: 99%

Volcanism and tectonism across the inner solar system: an overview

Platz

Byrne

Massironi

et al. 2014

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Volcanism and tectonism are the dominant endogenic means by which planetary surfaces change. This book, in general, and this overview, in particular, aim to encompass the broad range in character of volcanism, tectonism, faulting and associated interactions observed on planetary bodies across the inner solar system -a region that includes Mercury, Venus, Earth, the Moon, Mars and asteroids. The diversity and breadth of landforms produced by volcanic and tectonic processes are enormous, and vary across the inventory of inner solar system bodies. As a result, the selection of prevailing landforms and their underlying formational processes that are described and highlighted in this review are but a primer to the expansive field of planetary volcanism and tectonism. In addition to this extended introductory contribution, this Special Publication features 21 dedicated research articles about volcanic and tectonic processes manifest across the inner solar system. Those articles are summarized at the end of this review.

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“…The interior of Oanuava is occupied by an inner low that follows the general orientation of the corona, that is NE‐SW, forming a central elongated trough that lies below the surrounding plains but above the MPR. This characteristic causes this corona, in another coronae classification regarding the topographic relief [ DeLaughter and Jurdy , 1999] to be classified as calderic, that is, a corona with more than 50% of the interior lower than the surrounding plains.…”

Section: Study Of Oanuava Corona (325°s/2555°e) and Unnamed Corona mentioning

confidence: 99%

Plume channeling as one possible mechanism for the origin of multiple coronae on Venus: A case study from the Helen Planitia Quadrangle (V52)

López

2002

J.‐Geophys.‐Res.

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[1] Coronae are large volcanotectonic features formed in response to plume/diapir activity that have played an important role in the geodynamical evolution of Venus. Coronae are classified in terms of their morphology; one of the types is the so-called multiple coronae. Models that account for multiple coronae formation include the following: emplacement of several diapirs, the movement of the lithosphere over a stationary plume, and migration of a plume under a stationary lithosphere. This work presents the study of a multiple corona located in the Helen Planitia Quadrangle (V52) (Oanuava Corona) and another corona (unnamed) formed in the vicinity of Oanuava in order to test the viability of these models. Detailed structural mapping shows a migration of magmatic activity along the structure during corona formation and the development of a set of fractures in response to a local stress field. The latter is used as a time marker for the evolution of Oanuava and the unnamed coronae. We propose that this migration could be explained as the result of a sublithospheric lateral flow and ponding of a mantle plume or diapir into a zone of uplifted and thinned lithosphere (plume channeling) induced by the interaction of both coronae.INDEX TERMS: 6295 Planetology: Solar System Objects: Venus; 5480 Planetology: Solid Surface Planets: Volcanism (8450); 5475 Planetology: Solid Surface Planets: Tectonics (8149); KEYWORDS: Venus, multiple coronae, sublithospheric topography, plume channeling Citation: López, I., Plume channeling as one possible mechanism for the origin of multiple coronae on Venus: A case study from the

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Corona Classification by Evolutionary Stage

Cited by 27 publications

References 30 publications

Characterization and formation of polygonal fractures on Venus

Characterization and formation of polygonal fractures on Venus

Volcanism and tectonism across the inner solar system: an overview

Plume channeling as one possible mechanism for the origin of multiple coronae on Venus: A case study from the Helen Planitia Quadrangle (V52)

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