Paleohydrology of Eberswalde crater, Mars

Irwin, R. P.; Lewis, K. W.; Howard, A. D.; Grant, J. A.

doi:10.1016/j.geomorph.2014.10.012

Cited by 70 publications

(97 citation statements)

References 104 publications

(223 reference statements)

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“…Although they are found on geologic units mapped as Noachian in age, many Type‐3 craters may have formed in the Hesperian. This is certainly reflected in several detailed studies that have been conducted of Type‐3 craters, such as Gale (e.g., Grant et al, ; Le Deit et al, ) and Eberswalde (Irwin et al, ), both of which have been found to be Late Noachian to Hesperian in age. There are also several geologic attributes unique to Type‐3 craters.…”

Section: Discussionmentioning

confidence: 99%

An Assessment of Regional Variations in Martian Modified Impact Crater Morphology

2018

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Impact craters on Mars have been extensively modified by ancient geologic processes that may have included rainfall and surface runoff, snow and ice, denudation by lava flows, burial by eolian material, or others. Many of these processes can leave distinct signatures on the morphometry of the modified impact crater as well as the surrounding landscape. To look for signs of potential regional differences in crater modification processes, we conducted an analysis of different morphometric parameters related to modified impact craters located in the Margaritifer Sinus, Sinus Sabaeus, Iapygia, Mare Tyrrhenum, Aeolis, and Eridania quadrangles, including depth, crater wall slope, crater floor slope, the curvature between the interior wall and the crater floor slope, and the curvature between the interior wall and surrounding landscape. A Welch's t test analysis comparing these parameters shows that fresh impact craters (Type 4) have consistent morphologies regardless of their geographic location examined in this study, which is not unexpected. Modified impact craters both in the initial (Type 3) and terminal stages (Type 1) of modification also have statistically consistent morphologies. This would suggest that the processes that operated in the late Noachian were globally ubiquitous, and that modified craters eventually reached a stable crater morphology. However, craters preserved in advanced (but not terminal) stages of modification (Type 2) have morphologies that vary across the quadrangles. It is possible that these variations reflect spatial differences in the types and intensity of geologic processes that operated during the Noachian, implying that the ancient climate also varied across regions.

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Section: Discussionmentioning

confidence: 99%

An Assessment of Regional Variations in Martian Modified Impact Crater Morphology

2018

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“…The paucity of mineralogic evidence for in situ alteration of fan deposits [McKeown et al, 2013], the presence of hydrated silica (possibly opal [Carter et al, 2012]), and the persistence of olivine Geophysical Research Letters 10.1002/2017GL072660 [Stopar et al, 2006], when combined with the >20 Myr span of surface liquid water required by our data, suggest that climate conditions were cold and that intermittency further reduced liquid water interaction with soil. Intermittency is also suggested by multiple pulses of fan formation at Holden [Irwin et al, 2015], Gale, and Melas Chasma [Williams and Weitz, 2014]. Intermittency is also suggested by multiple pulses of fan formation at Holden [Irwin et al, 2015], Gale, and Melas Chasma [Williams and Weitz, 2014].…”

Section: Implications For Paleohydrology and Climatementioning

confidence: 93%

“…Prefluvial craters (which are overlain by fan deposits but that formed before the start of fluvial deposition [Irwin et al, 2015]) are excluded. Prefluvial craters (which are overlain by fan deposits but that formed before the start of fluvial deposition [Irwin et al, 2015]) are excluded.…”

Section: Introductionmentioning

confidence: 99%

Persistent or repeated surface habitability on Mars during the late Hesperian ‐ Amazonian

Kite

Sneed

Mayer

et al. 2017

Geophysical Research Letters

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Large alluvial fan deposits on Mars record relatively recent habitable surface conditions (≲3.5 Ga, Late Hesperian ‐ Amazonian). We find net sedimentation rate <(4–8) μm/yr in the alluvial fan deposits, using the frequency of craters that are interbedded with alluvial fan deposits as a fluvial‐process chronometer. Considering only the observed interbedded craters sets a lower bound of >20 Myr on the total time interval spanned by alluvial fan aggradation, >103‐fold longer than previous lower limits. A more realistic approach that corrects for craters fully entombed in the fan deposits raises the lower bound to >(100–300) Myr. Several factors not included in our calculations would further increase the lower bound. The lower bound rules out fan formation by a brief climate anomaly. Therefore, during the Late Hesperian ‐ Amazonian on Mars, persistent or repeated processes permitted habitable surface conditions.

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“…Large (>10 km 2 ), late‐stage Martian alluvial fans and river deltas provide evidence for surface liquid water on post‐Noachian Mars after about 3.5 Gya (Grant & Wilson, ; Irwin et al, ; Palucis et al, ; Williams & Weitz, ). However, by about 3.5 Gya most of the conditions favorable to the existence of surface liquid water no longer existed: much of Mars's atmosphere was lost before the end of the Noachian and the Martian dynamo shut down around the mid‐Noachian (Lillis et al, ; Pepin, ).…”

Section: Introductionmentioning

confidence: 99%

Effect of Mars Atmospheric Loss on Snow Melt Potential in a 3.5 Gyr Mars Climate Evolution Model

2018

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Post‐Noachian Martian paleochannels indicate the existence of liquid water on the surface of Mars after about 3.5 Gya (Irwin et al., 2015, https://doi.org/10.1016/j.geomorph.2014.10.012; Palucis et al., 2016, https://doi.org/10.1002/2015JE004905). In order to explore the effects of variations in CO2 partial pressure and obliquity on the possibility of surface water, we created a zero‐dimensional surface energy balance model. We combine this model with physically consistent orbital histories to track conditions over the last 3.5 Gyr of Martian history. We find that melting is allowed for atmospheric pressures corresponding to exponential loss rates of dP/d t∝t−3.73 or faster, but this rate is within 0.5σ of the rate calculated from initial measurements made by the Mars Atmosphere and Volatile EvolutioN (MAVEN) mission, if we assume all the escaping oxygen measured by MAVEN comes from atmospheric CO2 (Lillis et al., 2017, https://doi.org/10.1002/2016JA023525; Tu et al., 2015, https://doi.org/10.1051/0004-6361/201526146). Melting at this loss rate matches selected key geologic constraints on the formation of Hesperian river networks, assuming optimal melt conditions during the warmest part of each Mars year (Irwin et al., 2015, https://doi.org/10.1016/j.geomorph.2014.10.012; Kite, Gao, et al., 2017, https://doi.org/10.1038/ngeo3033; Kite, Sneed et al., 2017, https://doi.org/10.1002/2017GL072660; Stopar et al., 2006, https://doi.org/10.1016/j.gca.2006.07.039). The atmospheric pressure has a larger effect on the surface energy than changes in Mars's mean obliquity. These results show that initial measurements of atmosphere loss by MAVEN are consistent with atmospheric loss being the dominant process that switched Mars from a melt‐permitting to a melt‐absent climate (Jakosky et al., 2017, https://doi.org/10.1126/science.aai7721), but non‐CO2 warming will be required if <2 Gya paleochannels are confirmed or if most of the escaping oxygen measured by MAVEN comes from H2O.

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Paleohydrology of Eberswalde crater, Mars

Cited by 70 publications

References 104 publications

An Assessment of Regional Variations in Martian Modified Impact Crater Morphology

An Assessment of Regional Variations in Martian Modified Impact Crater Morphology

Persistent or repeated surface habitability on Mars during the late Hesperian ‐ Amazonian

Effect of Mars Atmospheric Loss on Snow Melt Potential in a 3.5 Gyr Mars Climate Evolution Model

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