Evidence for Middle Amazonian catastrophic flooding and glaciation on Mars

Rodriguez, J. A. P.; Gulick, V. C.; Baker, Victor R.; Platz, Thomas; Fairén, Alberto González; Miyamoto, H.; Kargel, Jeffrey S.; Rice, J. W.; Glines, N. H.

doi:10.1016/j.icarus.2014.06.008

Cited by 26 publications

(25 citation statements)

References 49 publications

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“…The outflow here and at other Amazonian outflow sites (e.g. [50]) took place after the opening of Valles Marineris, and after a possible disconnect between the Tharsis source area. This implies one of the following scenarios: (1) early outflow events did not release all groundwater pressure, which can be explained by closure of the cryosphere seal during the outflow event (e.g.…”

Section: Aquifer Pressurizationmentioning

confidence: 80%

“…Outflow channel activity was concentrated in the Hesperian, but continued throughout the Amazonian [50,63]. Early outflow events at Ophir and Lunae Plana in the Hesperian before the formation of Valles Marineris could be the result from recharge at higher elevation in Tharsis [27] and requires a confining layer, which we assume to be the cryosphere [14,15].…”

Section: Aquifer Pressurizationmentioning

confidence: 96%

“…Similarly, most circum-Cryse outflow channel activity peaked in the Hesperian, e.g. Kasei Valles (3.4 Gyr, [45]), although outflow events continued in the Amazonian [45,50]. Besides the outflow channels, lakes likely existed in this region in the early Hesperian (e.g.…”

Section: Chronological Frameworkmentioning

confidence: 96%

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Pressurized groundwater systems in Lunae and Ophir Plana (Mars): Insights from small-scale morphology and experiments

Marra

Hauber

Jong

et al. 2015

GeoResJ

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a b s t r a c tOutflow channels on Mars reveal the past presence of water, possibly released from pressurized groundwater reservoirs. We aim to improve our understanding of such outflow systems in order to better constrain past hydrological conditions on Mars. We investigate the morphology of possible pressurized groundwater outflow systems on Mars and compare them to landscape evolution experiments. These experiments show that incised channels, like the classic outflow channels, form in a last, erosional, stage in morphological development. This is preceded by the formation of sedimentary lobes due to rapid water loss by infiltration. On Mars, we observe similar morphologies related to different stages of groundwater outflow in Lunae and Ophir Plana. In the experiments, pits formed by the pressure of the groundwater, whereas the pits in the source regions of the outflow channels relate to the regional tectonic structure and are not formed by groundwater alone. Faulting, subsidence and collapse likely triggered outflow from a pressurized aquifer. This scenario is consistent with the presence of one or several cryosphere-confined aquifers from the Early Hesperian to at least the middle Amazonian. A pronounced spatial trend of larger and further developed outflow systems at lower elevations suggests that features ranging from small lobes to large outflow channels were sourced from a common aquifer or from aquifers with similar pressures. The required cryosphere indicates a cold climate and enables groundwater outflow even under atmospheric conditions unfavorable for sustained presence of liquid water.

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Section: Aquifer Pressurizationmentioning

confidence: 80%

Section: Aquifer Pressurizationmentioning

confidence: 96%

See 1 more Smart Citation

Pressurized groundwater systems in Lunae and Ophir Plana (Mars): Insights from small-scale morphology and experiments

Marra

Hauber

Jong

et al. 2015

GeoResJ

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“…For example, some investigations show evidence indicative of regional outflow channel formation during the Late Noachian (Warner et al, 2013a) and Early Amazonian (Rodriguez et al, 2011;Warner et al, 2013b). In a more recent study, Rodriguez et al (2014) investigated outflow channel exposures in southern circum-Chryse containing decameter-scale bedforms indicative of Middle Amazonian outflow channel formation associated with glaciation and catastrophic flooding events. Although these new investigations indicate a significant deviation from the putative, almost exclusive Late Hesperian age benchmark of outflow channel activity in circum-Chryse, this view still remains ingrained in Mars science literature (Coleman et al, 2007).…”

Section: Contents Lists Available At Sciencedirectmentioning

confidence: 99%

“…1a) comprise some of the largest outflow channels on Mars, and their excavation has been attributed to erosion by catastrophic floods (Baker, 1982(Baker, , 2009a(Baker, , 2009bKomatsu and Baker, 1997;Rodriguez et al, 2014), glaciers (Lucchitta, 1982(Lucchitta, , 2001Pacifici et al, 2009;Rodriguez et al, 2014), CO 2 -charged debris flows (Hoffman, 2000), H 2 O-charged debris flows (Nummedal and Prior, 1981;Tanaka, 1999;Rodriguez et al, 2006a), and/or lava flows (Schonfeld, 1976;Leverington, 2011;Hopper and Leverington, 2014). The analyses of Viking Orbiter era geochronologies led to a consensus that the Late Hesperian (3.61-3.37 Ga, (Werner and Tanaka 2011;Michael 2013)) comprised a period characterized by major hydrologic resurfacing on Mars, which resulted in the formation of the planet's major outflow channel systems (Scott and Tanaka, 1986;Rotto and Tanaka, 1995;Tanaka, 1997).…”

Section: Introductionmentioning

confidence: 99%