Sources of water for the outflow channels on Mars: Implications of the Late Noachian “icy highlands” model for melting and groundwater recharge on the Tharsis rise

Cassanelli, J. P.; Head, J. W.; Fastook, J. L.

doi:10.1016/j.pss.2015.01.002

Cited by 27 publications

(15 citation statements)

References 109 publications

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“…where H is ice thickness (m), k T is thermal conductivity of the ice (assumed to be 2.5 W m À1 K À1 ) (Cassanelli et al, 2015), and Q is basal heating (W m À2 ), equal to geothermal heat flux, G, plus any internal strain heating. Volumetric strain heating (P, W m À3 ) at depth can be calculated as (e.g., Lüthi et al, 2015)…”

Section: Estimation Of Temperatures At the Base Of The Vffmentioning

confidence: 99%

Recent Basal Melting of a Mid‐Latitude Glacier on Mars

et al. 2017

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Evidence for past basal melting of young (late Amazonian‐aged), debris‐covered glaciers in Mars' mid‐latitudes is extremely rare. Thus, it is widely thought that these viscous flow features (VFFs) have been perennially frozen to their beds. We identify an instance of recent, localized wet‐based mid‐latitude glaciation, evidenced by a candidate esker emerging from a VFF in a tectonic rift in Tempe Terra. Eskers are sedimentary ridges deposited in ice‐walled meltwater conduits and are indicative of glacial melting. We compare the candidate esker to terrestrial analogues, present a geomorphic map of landforms in the rift, and develop a landsystem model to explain their formation. We propose that the candidate esker formed during a transient phase of wet‐based glaciation. We then consider the similarity between the geologic setting of the new candidate esker and that of the only other candidate esker to be identified in association with an existing mid‐latitude VFF; both are within tectonic graben/rifts proximal to volcanic provinces. Finally, we calculate potential basal temperatures for a range of VFF thicknesses, driving stresses, mean annual surface temperatures, and geothermal heat fluxes, which unlike previous studies, include the possible role of internal strain heating. Strain heating can form an important additional heat source, especially in flow convergence zones, or where ice is warmer due to elevated surface temperatures or geothermal heat flux. Elevated geothermal heat flux within rifts, perhaps combined with locally‐elevated strain heating, may have permitted wet‐based glaciation during the late Amazonian, when cold climates precluded more extensive wet‐based glaciation on Mars.

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Section: Estimation Of Temperatures At the Base Of The Vffmentioning

confidence: 99%

Recent Basal Melting of a Mid‐Latitude Glacier on Mars

et al. 2017

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“…However, they are not distinguishable, no evidence preserved or observed, thus leads to rule out this possibility. Cassanelli et al () reported the late Noachian Icy Highlands, which describes about the distribution of ice at the surface. In such scenario, possible channel origins form the contact melting from ejecta (Weiss et al, ) or thermal anomaly of impacts and their ejecta over ice‐bearing terrains forms channels (Mangold, ).…”

Section: Discussionmentioning

confidence: 99%

Evidence for Multiple Superposed Fluvial Deposits Within Reuyl Crater, Mars

et al. 2020

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Reuyl is an 85‐km‐diameter crater located east of the Aeolis Dorsa region. We present results from geomorphic mapping and high‐resolution image analyses of Reuyl to understand the provenance of alluvial fans, superposed deposits, channels, and sinuous ridges. We distinguish 29 fans or other deposits associated with channels based on their characteristics. Two sinuous ridges are associated with the alluvial fans formed between the wall and peak region. On the southern floor, a sinuous ridge associated with an alluvial fan with channel inversion is orthogonally superposed by another wall‐originated fan deposit. On the western floor, a sinuous ridge associated with an alluvial fan is superposed by wall‐originated deposits. We also observe bajadas, stacked deposits, deposits with incised channels, and overlapping fan ridges, which suggest diverse and long‐lived depositional activity related to a fluvial environment. The central peak is surrounded by a mound deposit with several discontinuous channels. One large fan from the western wall appears more intact than the others, being less eroded and lacking ridges. Reuyl aged as ~3.63 Ga, whereas the first‐order analysis of the fan deposits implies ~3.5 Ga and the large intact deposit is estimated to belong to the Amazonian epoch. We suggest that Reuyl crater likely witnessed and recorded the transition from alluvial fan to large younger intact deposits, which possibly suggests a decrease in water/volatile‐related activity and/or change in sediment supply. Overall, the diverse superposed fan deposits within Reuyl reveal noncoeval activity and provide comprehensive evidence for long‐lived fluvial activity during the post‐Noachian epoch.

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“…Furthermore, as suggested by Hanna and Phillips (2005), the break of the cryosphere by a pressurized aquifer is unlikely unless it is not taken as an a priori condition. The occurrence of a global pressurized aquifer alimented by basal melting of South polar cap is contrasted by the very low hydrostatic head between Chryse and polar regions (Russell and Head, 2007;Cassanelli et al, 2015). Source of groundwater from ice sheets on Tharsis rise can potentially generate a higher hydrostatic head (Harrison and Grimm, 2004).…”

Section: Discussionmentioning

confidence: 99%

“…Source of groundwater from ice sheets on Tharsis rise can potentially generate a higher hydrostatic head (Harrison and Grimm, 2004). However, this model does not account for enough water needed to carve the outflow channels (Cassanelli et al, 2015) as well as to break the cryosphere in case of icy scenario for Mars (Forget et al, 2013;Wordsworth et al, 2013). Mechanisms based on aquifer discharge therefore cannot explain spatially extensive collapse and cryosphere fracturing.…”

Section: Discussionmentioning

confidence: 99%