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basin dome terrain. After sufficient crustal thickening has occurred, new lithosphere is generated causing gravitational collapse, producing the extensional features of tessera, such as extensive grabens. During this collapse, decompression causes partial melting, producing the intratessera volcanism seen within the larger regions of tessera terrain. This model requires that the material comprising tessera terrain is continental in nature. Future missions to Venus to sample surface compositions are necessary to support this model. This model does not currently explain how a global subduction event could cause the delamination of the entire mantle lithosphere, leaving only low density crust behind.
183:
Multiple models have been put forward to explain the formation of tessera terrain. Models of formation by mantle downwelling and pulsating continents are the most currently accepted models. A model of formation due to a lava pond via bolide impact was put forth, although it has not currently gained much traction in the scientific community due to skepticism of the ability of a bolide impact to generate sufficient melt. A model of formation due to mantle plumes (upwelling) was persistent for many years, however, it has since been abandoned due to its contradictory prediction of sequences of extension versus the observed cross cutting relationships.
64:. Tesserae often represent the oldest material at any given location and are among the most tectonically deformed terrains on Venus's surface. Diverse types of tessera terrain exist. It is not currently clear if this is due to a variety in the interactions of Venus's mantle with regional crustal or lithospheric stresses, or if these diverse terrains represent different locations in the timeline of crustal plateau formation and fall. Multiple models of tessera formation exist and further extensive studies of Venus's surface are necessary to fully understand this complex terrain.
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120:. Tesserae are exposed almost entirely within Venus's crustal plateaus. Tessera inliers, regions of tessera not found within current crustal plateaus are thought to represent regions of collapsed crustal plateaus. Large regions of tessera terrain are labelled based on their latitude. Regions in the equatorial and southern latitudes are labelled as "regio" while regions in the northern latitudes are labelled as "tesserae."
222:
171:
280:, also known as honeycomb terrain, consists of curved ridges and troughs that form a pattern analogous to an egg carton. These structures represent multiple phases of deformation, and are considered the most complex appearing style of tessera. Basin and dome terrain is typically found within the center of crustal plateaus.
212:
impact on a thin lithosphere rises to the surface to form a lava pond. Convection throughout the lava pond resulted in surface deformation that created tessera terrain. Isostatic rebound of the solidified pond creates a crustal plateau structure. This model does not currently explain how convection
273:
tectonic fabrics on Earth. It consists of two main structures: synchronous folds and small, 5 to 20 km long graben that cross cut the folds perpendicularly. Unlike many other types of tessera terrain, S-C terrain indicates a simple, rather than complex deformation history in which deformation
229:
In the pulsating continents model, differentiated, low density crust survives early global subduction events forming continental regions. These regions undergo compression due to heating from the surrounding mantle, forming the compressional features of tessera, such as fold and thrust belts, and
182:
on Venus. Tessera
Terrain does not participate in the global resurfacing events of Venus. It was thought by many researches that the tesserae might form a global "onion skin" of sorts, and extended beneath Venus's regional plains. However, the currently accepted models support regional formation.
245:
is easily recognizable by its well defined linear fabrics. This type of terrain is composed of long ridges and valleys, greater than 100 km long, that are cross cut by minor extensional fractures that run perpendicular to the fold axes of the ridges. This likely formed due to unidirectional
199:
In the downwelling model, mantle downwelling, possibly due to mantle convection, causes compression and thickening of the crust, creating the compressional elements of tessera terrain. Isostatic rebound occurs due to the crustal thickening. After downwelling ends, a delamination event within the
238:
Individual patterns of tessera terrain record the variations in interactions of the mantle with local regional stresses. This variation manifests itself in a wide array of diverse terrain types. Multiple types of sampled tessera terrain are below, however, they are not meant as a classification
286:
is composed of multiple graben and fractures that trend in many directions, but radiate in a star-like pattern. This pattern is thought to be due to doming underneath previously deformed and fractured areas, in which the local uplift causes the radiating pattern.
262:
is characterized by ribbons and folds that are typically orthogonal to one another. Ribbons are long and narrow extensional troughs that are separated by narrow ridges. Ribbon terrain can be found both in large crustal plateaus and within tessera inliers.
111:
10 sq mi), and occur mostly within a few extensive provinces. They are heavily concentrated between 0E and 150E. These longitudes represent a large area between a crustal extension center in the
256:
flows found on Earth, with long curving ridges. It is thought that this terrain may be formed due to displacement and deformation due to movement of the material beneath these crustal pieces.
95:
Mission, in which the majority of Venus's surface was mapped in high resolution (~100 m/pixel). Future missions to Venus would allow for further understanding of tessera terrain.
451:
Barsukov, V.L., et al, "The geology of Venus according to the results of an analysis of radar images obtained by Venera-15 and Venera-16 Preliminary data", Geokhimiya, Dec. 1984
200:
mantle produces extensional elements of tessera. This model does not currently explain tessera's location within crustal plateaus, and instead predicts a domical shape.
274:
due to widespread motion on Venus is widely distributed. This type of terrain also indicates that strike-slip movement on Venus's surface is possible.
161:
Interpretive outline of tessera terrain (white outline) imposed on "GIS Map of Venus" (GIS Map of Venus source: USGS Astrogeology
Science Center)
365:
Hansen, Vicki; Willis, James (1998). "Ribbon
Terrain Formation, Southwestern Fortuna Tessera, Venus: Implications for Lithosphere Evolution".
124:
36:
Tessera terrain in the
Maxwell Montes seen in white on the right of the image. Eastern edge of Lakshmi Planum seen in gray on the left.
679:
768:
Hansen, V.L.; Lopez, I. (2009). "Implications of Venus
Evolution Based on Ribbon Tessera Relation Within Five Large Regional Areas".
876:
Hansen, Vicki; Willis, James (1996). "Structural
Analysis of a Sampling of Tesserae: Implications for Venus Geodynamics".
311:
Bindschadler, Duane; Head, James (1991). "Tessera
Terrain, Venus: Characterization and Models for Origin and Evolution".
671:
91:, pronounced par-key'yet), later known as "tesserae." The most recent data concerning tessera terrain comes from the
270:
461:
Head, James (1990). "Venus Trough and Ridge
Tessera: Anolog to Earth Oceanic Crust Formed at Spreading Centers?".
917:
526:
76:
826:"Geologic constraints on crustal plateau surface histories, Venus: The lava pond and bolide impact hypotheses"
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orbiters revealed these regions to be chaotically tiled terrain, which Soviet scientists named "ΠΏΠ°ΡΠΊΠ΅Ρ" (
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320:
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Hansen, Vicki; Banks, Brian; Ghent, Rebecca (1999). "Tessera terrain and crustal plateaus, Venus".
174:
Model of crustal plateau and tessera terrain formation via mantle downwelling after
Gilmore (1998).
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Ivers, Carol; McGill, George. "Kinematics of a
Tessera Block in the Vellamo Planitia Quadrangle".
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113:
584:"Pulsating continents on Venus: An explanation for crustal plateaus and tessera terrains"
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518:
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428:
378:
324:
624:
Campbell, Bruce; Campbell, Donald; Morgan, Gareth; Carter, Lynn; Nolan, Micael (2015).
911:
394:
626:"Evidence for crater ejecta on Venus tessera terrain from Earth-based radar images"
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136:
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Tesserae are recognized as covering 7.3% of Venus's surface, approximately 3.32
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could transmit enough force to deform several kilometers of brittle material.
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57:
482:
84:
80:
897:
668:
Venus II : Geology, Geophysics, Atmosphere, and Solar Wind Environment
386:
195:
Model of crustal plateau and tessera terrain formation after Hansen (2006).
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detected regions of anomalous radar properties and high backscatter. Using
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825:
437:
412:
253:
785:"Style and sequence of extensional structures in tessera terrain, Venus"
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Turcotte, D.L. (1993). "An episodic hypothesis for Venusian tectonics".
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88:
809:
784:
751:
411:
Hansen, Vicki; Phillips, Roger; Willis, James; Ghent, Rebecca (2000).
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716:
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Ivanov, Mikhail; Head, James (2011). "Global Geologic Map of Venus".
209:
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49:
31:
123:
A comprehensive list of regiones and tesserae can be found under
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Gilmore, Martha; Collins, Geoffrey; Ivanov, Mikhail (1998).
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scheme, and instead emphasize the variety of terrain types.
527:
10.1130/0091-7613(1999)027<1071:ttacpv>2.3.co;2
413:"Structures in tessera terrain, Venus: Issues and answers"
666:
Bougher, Steven; Hunten, Donald; Phillips, Roger (1997).
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In the lava pond via giant impact model, melt due to a
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761:
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Tesserae represent an ancient time of globally thin
695:Solomon, S.C. (1993). "The geophysics of Venus".
269:is named such due to its geometric similarity to
127:. Some well explored regions of tessera include:
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48:) is a region of heavily deformed terrain on
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52:, characterized by two or more intersecting
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252:is named such due to its resemblance to
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770:Lunar and Planetary Science Conference
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125:List of geological features on Venus
116:and a crustal convergence center in
591:Earth and Planetary Science Letters
27:Region of deformed terrain on Venus
582:Romeo, I.; Turcotte, D.I. (2008).
25:
830:Journal of Geophysical Research
789:Journal of Geophysical Research
732:Journal of Geophysical Research
463:Journal of Geophysical Research
417:Journal of Geophysical Research
313:Journal of Geophysical Research
1:
653:10.1016/j.icarus.2014.11.025
60:, and subsequent high radar
18:Tessera (Venusian geography)
672:University of Arizona Press
542:Planetary and Space Science
348:Lunar and Planetary Science
934:
611:10.1016/j.epsl.2008.09.009
234:Variety of tessera terrain
225:Pulsating continents model
204:Lava pond via giant impact
107:10 square kilometres (1.28
562:10.1016/j.pss.2011.07.008
603:2008E&PSL.276...85R
554:2011P&SS...59.1559I
483:10.1029/jb095ib05p07119
898:10.1006/icar.1996.0159
824:Hansen, Vicki (2006).
387:10.1006/icar.1998.5897
278:Basin and Dome Terrain
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73:Pioneer Venus Orbiter
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851:10.1029/2006JE002714
438:10.1029/1999je001137
217:Pulsating continents
890:1996Icar..123..296H
842:2006JGRE..11111010H
801:1998JGR...10316813G
744:1993JGR....9817061T
738:(E9): 17061β17068.
709:1993PhT....46g..48S
645:2015Icar..250..123C
519:1999Geo....27.1071H
475:1990JGR....95.7119H
429:2000JGR...105.4135H
379:1998Icar..132..321H
325:1991JGR....96.5889B
836:(E11010): E11010.
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810:10.1029/98JE01322
752:10.1029/93je01775
548:(13): 1559β1600.
513:(12): 1071β1074.
469:(B5): 7119β7132.
423:(E2): 4135β4152.
333:10.1029/90jb02742
319:(B4): 5889β5907.
250:Lava Flow Terrain
54:tectonic elements
16:(Redirected from
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918:Geology of Venus
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639:: 123β130.
267:S-C Terrain
187:Downwelling
180:lithosphere
137:Alpha Regio
68:Exploration
62:backscatter
291:References
152:Ovda Regio
142:Beta Regio
58:topography
166:Formation
99:Locations
85:Venera 16
81:Venera 15
912:Category
395:18119376
254:Pahoehoe
93:Magellan
46:tesserae
44:(plural
886:Bibcode
838:Bibcode
797:Bibcode
740:Bibcode
705:Bibcode
641:Bibcode
599:Bibcode
550:Bibcode
515:Bibcode
507:Geology
471:Bibcode
425:Bibcode
375:Bibcode
321:Bibcode
89:parquet
56:, high
42:tessera
878:Icarus
678:
633:Icarus
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367:Icarus
210:bolide
629:(PDF)
587:(PDF)
391:S2CID
50:Venus
676:ISBN
83:and
894:doi
882:123
846:doi
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805:doi
793:103
748:doi
713:doi
649:doi
637:250
607:doi
595:276
558:doi
523:doi
479:doi
433:doi
421:105
383:doi
371:132
329:doi
271:S-C
77:SAR
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