Geometry, stratigraphy and evidences for fluid expulsion within Crommelin crater deposits, Arabia Terra, Mars

Franchi, Fulvio; Rossi, Angelo Pio; Pondrelli, M.; Cavalazzi, Barbara

doi:10.1016/j.pss.2013.12.013

Cited by 30 publications

(71 citation statements)

References 61 publications

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“…ELDs reach their maximum thickness of more than 2 km roughly in correspondence of the crater central peak (Franchi et al, 2014). The most significant morphologies associated with these deposits are represented by hundreds of meters large mounds made of breccia and fissure ridges that can be as long as hundreds of meters to several kilometers.…”

Section: Sedimentary Processesmentioning

confidence: 97%

“…Whether some of those are reflecting spring-related deposition rather than mud expulsion driven by subsurface fluids is subject to further work (e.g., Pondrelli et al, 2011a;Franchi et al, 2014). The two processes might be co-existing.…”

Section: Sedimentary Processesmentioning

confidence: 99%

“…HRSC-based computations on crater bulges (Crommelin Crater and Firsoff Crater in particular) in Arabia Terra allowed quantifying the geometry of the Equatorial Layered Deposits (ELDs, Franchi et al, 2014). ELDs reach their maximum thickness of more than 2 km roughly in correspondence of the crater central peak (Franchi et al, 2014).…”

Section: Sedimentary Processesmentioning

confidence: 99%

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Quantifying geological processes on Mars—Results of the high resolution stereo camera (HRSC) on Mars express

Jaumann

Tirsch

Hauber

et al. 2015

Planetary and Space Science

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a b s t r a c tThis review summarizes the use of High Resolution Stereo Camera (HRSC) data as an instrumental tool and its application in the analysis of geological processes and landforms on Mars during the last 10 years of operation. High-resolution digital elevations models on a local to regional scale are the unique strength of the HRSC instrument. The analysis of these data products enabled quantifying geological processes such as effusion rates of lava flows, tectonic deformation, discharge of water in channels, formation timescales of deltas, geometry of sedimentary deposits as well as estimating the age of geological units by crater size-frequency distribution measurements. Both the quantification of geological processes and the age determination allow constraining the evolution of Martian geologic activity in space and time. A second major contribution of HRSC is the discovery of episodicity in the intensity of geological processes on Mars. This has been revealed by comparative age dating of volcanic, fluvial, glacial, and lacustrine deposits.Volcanic processes on Mars have been active over more than 4 Gyr, with peak phases in all three geologic epochs, generally ceasing towards the Amazonian. Fluvial and lacustrine activity phases spread a time span from Noachian until Amazonian times, but detailed studies show that they have been interrupted by multiple and long Contents lists available at ScienceDirect

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Section: Sedimentary Processesmentioning

confidence: 97%

Section: Sedimentary Processesmentioning

confidence: 99%

Section: Sedimentary Processesmentioning

confidence: 99%

See 1 more Smart Citation

Quantifying geological processes on Mars—Results of the high resolution stereo camera (HRSC) on Mars express

Jaumann

Tirsch

Hauber

et al. 2015

Planetary and Space Science

Self Cite

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“…Rossi et al, 2008;Pondrelli et al, 2011;Michalski et al, 2013;Franchi et al, 2014). CRISM imagery of martian surface suggests that upwelling fluids triggered evaporite minerals deposition (e.g.…”

Section: Quartz-rich Rocks On Marsmentioning

confidence: 99%

“…Squyres and Knoll, 2005). Mounds and furrows detected within Crommelin crater on Mars have been interpreted as morphological evidence of subsurface fluids expulsion (Franchi et al, 2014). Interactions of deep fluids with basaltic rocks triggered the mobilization of silica from volcanic glass McLennan, 2003), and the formation of hematite and Mg-sulfate rich deposits (Christensen et al, 2000;Hynek et al, 2002;McLennan, 2003).…”

Section: Quartz-rich Rocks On Marsmentioning

confidence: 99%

Origin of John’s Stone: A quartzitic boulder from the site of the 1908 Tunguska (Siberia) explosion

Bonatti

Breger

Rocco

et al. 2015

Icarus

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Large‐scale fluid‐deposited mineralization in Margaritifer Terra, Mars

Thomas

Potter-McIntyre

Hynek

2017

Geophysical Research Letters

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Mineral deposits precipitated from subsurface‐sourced fluids are a key astrobiological detection target on Mars, due to the long‐term viability of the subsurface as a habitat for life and the ability of precipitated minerals to preserve biosignatures. We report morphological and stratigraphic evidence for ridges along fractures in impact crater floors in Margaritifer Terra. Parallels with terrestrial analog environments and the regional context indicate that two observed ridge types are best explained by groundwater‐emplaced cementation in the shallow subsurface and higher‐temperature hydrothermal deposition at the surface, respectively. Both mechanisms have considerable astrobiological significance. Finally, we propose that morphologically similar ridges previously documented at the Mars 2020 landing site in NE Syrtis Major may have formed by similar mechanisms.

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Geometry, stratigraphy and evidences for fluid expulsion within Crommelin crater deposits, Arabia Terra, Mars

Cited by 30 publications

References 61 publications

Quantifying geological processes on Mars—Results of the high resolution stereo camera (HRSC) on Mars express

Quantifying geological processes on Mars—Results of the high resolution stereo camera (HRSC) on Mars express

Origin of John’s Stone: A quartzitic boulder from the site of the 1908 Tunguska (Siberia) explosion

Large‐scale fluid‐deposited mineralization in Margaritifer Terra, Mars

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