Structural attitudes of large scale layering in Valles Marineris, Mars, calculated from Mars Orbiter Laser Altimeter data and Mars Orbiter Camera imagery

Fueten, Frank; Stesky, Robert; MacKinnon, Paula

doi:10.1016/j.icarus.2004.11.010

Cited by 30 publications

(28 citation statements)

References 22 publications

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“…Extracting topographic profiles along transects D4 and D5 we estimate bench dip at about 2°, ignoring areas with accumulations of darker material at the base of cliffs (where thermal inertia was $400-500 tiu, suggesting very coarse sand or perhaps indurated material). We verify this estimate by selecting locations on a bench we believe to be the bestexposed bed surface and best-fitting a plane using the method of Fueten et al (2005Fueten et al ( , 2008 and Okubo (2010). The orientation of a plane with 99.69% goodness of fit to the points strikes at 170.4 ± 10.5°and has a dip of 2 ± 1° (Fig.…”

Section: Topographic Analysismentioning

confidence: 89%

Topographic, spectral and thermal inertia analysis of interior layered deposits in Iani Chaos, Mars

Sefton‐Nash

Catling

Wood

et al. 2012

Icarus

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a b s t r a c tWe present an analysis of Interior Layered Deposits (ILDs) in Iani Chaos using visible, infrared, hyperspectral and topographic datasets acquired by instruments aboard NASA's Mars Global Surveyor, Mars Odyssey, Mars Reconnaissance Orbiter and ESA's Mars Express spacecraft. We focus on four main regions where ILDs outcrop in Iani Chaos. Deposits span a $2 km range of elevations and exhibit moderate to high albedos, layering at sub-decameter scales, thermal inertias of 300-800 J m À2 K À1 s À1/2 and a range of surface textures. Thermal inertia calculations use slope and azimuth corrections from High Resolution Stereo Camera (HRSC) topography. Spectral features in hyperspectral data acquired by NASA's Compact Reconnaissance Imaging Spectrometer for Mars (CRISM) suggest that gypsum (CaSO 4 Á2H 2 O) and kieserite (MgSO 4 ÁH 2 O) are present in most deposits. We report absorptions typically exhibited by alunite (KAl 3 (SO 4 ) 2 (OH) 6 ) and jarosite KFe 3þ 3 ðOHÞ 6 ðSO 4 Þ 2 as well as a number of features that may be attributable to a wide range of mono-and polyhydrated sulphates and hydroxyl-sulphates bearing a number of cations, including Mg 2+ , Fe 2+ , Fe 3+ and Ca 2+ . Spectral features similar to those of ammonium sulphates may also be present.Analysis of a HiRISE stereo DEM shows planar layering in some ILDs, favouring a sedimentary deposition origin. Stratigraphic mapping of hydration and sulphate spectral features in flat ILDs in central Iani Chaos suggest that specific elevation intervals in the stratigraphic column were subject to different levels of hydration, perhaps during episodes of water table elevation. This is consistent with formation models for ILDs and hydrological modelling. Geomorphic characteristics of deposits in northern and southern Iani Chaos suggest their relatively recent exhumation and significant erosion by aeolian processes. We conclude that any formation theory for ILDs in Iani Chaos should support mechanisms for different hydration states at different stratigraphic elevations and subsequent significant aeolian erosion, burial and reexposure.

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Section: Topographic Analysismentioning

confidence: 89%

Topographic, spectral and thermal inertia analysis of interior layered deposits in Iani Chaos, Mars

Sefton‐Nash

Catling

Wood

et al. 2012

Icarus

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“…(3) Only a thin mantle of dust covers the chasma rim, though wind could have carried and deposited the dust elsewhere on the planet. So although surface erosion by water or McCauley et al (1972); Sharp (1973); Lucchitta (1979) Collapse by removal of water or magma Sharp (1973); Courtillot et al (1975); Schonfeld (1979); Tanaka and Golombek (1989); Spencer and Fanale (1990); Schultz (1998); Schultz and Lin (2001); Fueten et al (2005); Rodriguez et al (2006); Rossi et al (2008) Tectonic rifting Sharp (1973); Blasius et al (1977); Frey (1979); Masson (1977Masson ( , 1985; Schonfeld (1979); Anderson and Grimm (1998); Schultz (1991Schultz ( , 1995; Chadwick and Lucchitta (1993); Peulvast and Masson (1993); Mége and Masson (1996); Peulvast et al (2001); Wilkins and Schultz (2003); Bleamaster (2009) Combination of mechanisms Lucchitta et al (1992); Tanaka (1997); Schultz (1998); Lucchitta and Chapman (2002); Montgomery and Gillespie (2005); Montgomery et al (2009) wind was undoubtedly important in other canyons (Table 1), it is unlikely to be the main agent that formed Hebes Chasma. The tectonic rifting hypothesis invokes an origin by north-south tectonic extension, forming Hebes Chasma as a graben (Fig.…”

Section: Previous Hypotheses For Formation Of Chasmatamentioning

confidence: 99%

Modeling the collapse of Hebes Chasma, Valles Marineris, Mars

Jackson¹,

Adams²,

Dooley³

et al. 2011

Geological Society of America Bulletin

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Physical modeling and detailed mapping of Hebes Chasma provide new insights into the crustal composition and origin of the Valles Marineris region of equatorial Mars.Hebes Chasma is a 315-km-long and 8-kmdeep closed depression containing distinctive landforms that include diapirs and extensive allochthonous fl ows that end in pits. A central puzzle of Hebes Chasma is how and where 10 5 km 3 of missing material disappeared. Our physical models tested the hypothesis that the chasma formed by collapse and removal of material from below. Gravity-driven collapse in the models reproduced all the chasma's main landforms as subsidence evolved from early sagging of the upper surface, to inward collapse and removal of material, to emergence of diapirs and low-gradient fl ows. The models and geologic evidence suggest that Hebes Mensa arched upward diapirically and raised deep stratigraphy almost level with the chasma rim. If the chasma indeed collapsed by subsurface drainage as occurred in the models, the upper 8-10 km of deposits at Hebes must have been solid to depths of ~5 km but viscous at greater depths. The materials removed could not have consisted mainly of basalt fl ows; instead, they probably were a mixture of hydrated and nonhydrated salts, water ice, liquid water, and insoluble (likely basaltic) particles. The proportions of these constituents are unknown but constrained because the material drained from the subsiding chasma and apparently contributed to the outburst fl oods released down neighboring Echus Chasma and Kasei Valles.

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“…wr.usgs.gov/), and characterizing the styles, extent, and timing of deformation within these deposits). Accordingly, much work has been conducted to characterize regional bedrock and deformational structure using topography derived from data sets such as HRSC (Fueten et al, 2006(Fueten et al, , 2008 and MOLA (Fueten et al, 2005). Results from these investigations have identified several locales that call for further structural mapping at yet higher resolutions in order to provide more detailed characterizations of the local structure and thereby improve current understanding of the area's geologic history.…”

Section: Faulting and Folding Of Layered Sedimentary Depositsmentioning

confidence: 99%