Tectonics of Syrtis Major Planum on Mars

Raitala, J.; Kauhanen, K.

doi:10.1007/bf00117193

Cited by 8 publications

(5 citation statements)

References 6 publications

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“…Some of the fractures are covered to the south by lava flows from Syrtis Major (e.g., Raitala and Kauhanen, 1989). No other major volcanic edifices have been identified near the Nili Fossae to date.…”

Section: Introductionmentioning

confidence: 96%

Evidence for extensive, olivine-rich bedrock on Mars

Hamilton¹,

Christensen²

2005

Geol

197

213

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Color infrared observations of an area around the Nili Fossae acquired by the Mars Odyssey thermal emission imaging system have been used to map the regional distribution and geologic context of olivine-rich materials that first were identified from Mars Global Surveyor thermal emission spectrometer data. Spectral, thermal, geomorphic, and topographic data demonstrate that the majority of olivine-rich material is in the form of inplace layered rock covering an area roughly four times larger than previously recognized. Some high olivine concentrations are associated with spatially small areas dominated by sediments. We favor olivine-rich basalts as the origin of the observed olivine enrichment, although several hypotheses are viable. Figure 1. Decorrelation stretched mosaic of study region. Bands 9 (12.57 m, 796 cm ؊1 ), 7 (11.04 m, 906 cm ؊1 ), and 5 (9.35 m, 1070 cm ؊1 ) are displayed as red, green, and blue, respectively. Olivinerich exposures are magenta to purple-blue. Black box denotes the location of Figure 2A.

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Section: Introductionmentioning

confidence: 96%

Evidence for extensive, olivine-rich bedrock on Mars

Hamilton¹,

Christensen²

2005

Geol

197

213

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“…(2) What is the nature of the wrinkle ridge pattern and how are wrinkle ridges, calderas, and volcanic deposits related in space and time? (3) Is Syrtis Major purely constructional as proposed by Schaber [1982] or are the wrinkle ridges of Syrtis Major related to subsidence or formation of a “megacaldera” [ Raitala and Kauhanen , 1989]? (4) What is the nature of Syrtis Major as a volcanic structure (i.e., edifice or regional plains)?…”

Section: Introductionmentioning

confidence: 99%

The Syrtis Major volcanic province, Mars: Synthesis from Mars Global Surveyor data

2004

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[1] We investigated the geology, stratigraphy, morphology, and topography of Syrtis Major, one of the large Hesperian-aged volcanic provinces on Mars. New data from the Mars Global Surveyor (MGS) and Odyssey spacecraft allowed us to study Syrtis Major in unprecedented detail. On the basis of Mars Orbiter Laser Altimeter (MOLA) data we estimated the thickness of Syrtis Major lavas to be on the order of $0.5-1.0 km, their volume being $1.6-3.2 Â 10 5 km 3 . MOLA data also show that the calderas of Nili and Meroe Patera are located within a large N-S elongated central depression and are on the order of 2 km deep. MOLA data further indicate that the slopes of the flanks of the shield are (1°. These very gentle slopes are similar to other Martian highland paterae such as Amphitrites, Tyrrhena, and Syria Planum but are much smaller than slopes measured on the flanks of large Martian shield volcanoes such as Olympus, Elysium, Ascraeus, and Arsia Mons. At kilometer-scale baselines, the surface of the Syrtis Major Formation is smoother than the surrounding highland plains but rougher than the floor of Isidis. We propose that the differences in surface roughness and wrinkle ridge patterns between Isidis Planitia and Syrtis Major are probably caused by additional sedimentation in the impact basin. Both the wrinkle ridge pattern and topography of Syrtis Major are interpreted to be consistent with a gravitational collapse of the southeastern sector of Syrtis Major. Recently a model has been proposed to explain the low elevation of the Isidis rim in the Syrtis Major region [e.g., Tanaka et al., 2002]. This model calls on catastrophic erosion of the rim that is triggered by the emplacement of sills, which interacted with a volatile-rich substrate. We used MOLA data from nearby terrains of the Isidis rim to investigate the Isidis rim in locations where it has supposedly been eroded. On the basis of our investigation we conclude that the smooth morphology and relatively low topography of the Isidis rim in the Syrtis Major region can be best explained by initial heterogeneities in topography and flooding with lavas, together with some erosion and/or tectonic modification of the original rim. New crater counts show that Syrtis Major is of Early Hesperian age (N(5) = 154), older than in the geologic map of Greeley and Guest [1987]. On the basis of inspection of all available Mars Orbiter Camera (MOC) images we identified several terrain types and developed a stratigraphic sequence for Syrtis Major. Large-scale erosional modification (e.g., deflation) of the Syrtis Major lavas and/or tephra deposits and redistribution of eolian material are evident in numerous MOC images.

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“…The regularity of the small ridge spacing has been explained by elastic buckling of the crust under horizontal stresses (Banerdt and Golombek, 1988). This be the case because the Venera data suggest that most of the individual ridges are located on crests of local high subbelts (Raitala and Kauhanen, 1990). Small Cytherean ridges resemble wrinkle ridges seen on other terrestrial planets, showing a similar distinct accumulation of individual ridges on a broad mare arch (Watters, 1988).…”

Section: Subbelt Ridgesmentioning

confidence: 87%

“…Plotting ridge height versus ridge width can be used to reveal secondary ridge patterns and to determine the main ridge directions. An arch ridge pattern has also been found on Venus (Raitala and Kauhanen, 1990), but it is difficult to establish a tectonic origin on the basis of this method because of the inadequate resolution of the Venera radar imagery.…”

Section: Classification Of Ridge Beltsmentioning

confidence: 99%

“…Corona-like rings (protocoronae or arachnoids) and mountainous hills are mostly found at the junctions of ridge belts (Aspasia Patera, Razia Patera) or in the middle of them (Tituba Patera, Hallgerda Mons), but sometimes also as separate formations (Neyterkob Corona, Wurunsemu Tholus) which are connected to an adjacent ridge belt in a complex way (Raitala and Kauhanen, 1990). The Venera resolution does not allow us to determine the actual timing between the volcanic formations and ridge belts.…”

Section: Ridge Belts Of Ganiki Planitiamentioning

confidence: 99%

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Ridge belt tectonics of Ganiki Planitia on Venus

Raitala

Kauhanen

1991

Earth Moon Planet

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The main major ridge belts of Ganiki Planitia on Venus (Laftma, Ahsonnutli and Pandrosos Dorsa) are part of the fan-shaped ridge belt complex along the 200 ° parallel of longitude. These ridge belts with evidence of crustal shortening support the idea of a large-scale E-W compression. The ridge belt patterns indicate a N-S shear component. These forces are explained by a triangular planitia area which compressed by surrounding terrains. The crustal shortening and ridge belt formation indicates compressional plate movement stresses in the uppermost lithosphere.Three sizes of ridge belt structure are to be found within Ganiki Planitia. (1) The ridge belt spacing of 200-400 km can be used to estimate the depth of the major uppermost homogeneous layer of Venus. There are numerous volcanic coronae, paterae and montes located along the main ridge belts or at their junctions. (2) Mid-size ridge groups or subbelts are to be found within the major ridge belts. These are formed by more local responses to tectonic stresses in the stratified uppermost crust. A wavelength of 40-70 km can be seen as a result of bending of the crustal strata and may relate to its thickness. (3) Small individual ridges are connected with most local stresses, defining places where the surface layers broke along the crests of large ridge belts or mid-scale subbelts. Radial and concentric mare ridge-like structures around eoronae indicate that corona formation was effective at a sufficiently close vicinity to fault the surface.

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Tectonics of Syrtis Major Planum on Mars

Cited by 8 publications

References 6 publications

Evidence for extensive, olivine-rich bedrock on Mars

Evidence for extensive, olivine-rich bedrock on Mars

The Syrtis Major volcanic province, Mars: Synthesis from Mars Global Surveyor data

Ridge belt tectonics of Ganiki Planitia on Venus

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