Local late Amazonian boulder breakdown and denudation rate on Mars

Haas, Tjalling de; Hauber, Ernst; Kleinhans, Maarten G.

doi:10.1002/grl.50726

Cited by 34 publications

(35 citation statements)

References 49 publications

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“…Data point at 0.1 Myr is for degradation of Concepción crater (class 1) as described in the text and represents the maximum short‐term rate in the modern era. Erosion rate marked M1 includes our classes 2 and 3 crater degradation rates at Meridiani Planum, plus erosion of an alluvial fan [ de Haas et al ., ], and lightly cratered layered terrain [ Malin and Edgett , ; McEwen et al ., ]. Erosion rates marked M2 are from our class 4–6 degradation rates for craters in Meridiani Planum.…”

Section: Discussion: Erosion Rate Changes With Timementioning

confidence: 99%

“…Erosion of ejecta blocks to liberate blueberries around Concepción crater has been estimated at about 1 m/Ma in the past 10 ka [ Golombek et al ., ], and infill has been estimated at 10 m/Ma (section 7.1). Erosion and smoothing of boulders on a ~1 Ma inactive alluvial fan has been estimated at ~1 m/Myr [ de Haas et al ., ]. Abrasion rates of 1–10 m/Myr have been estimated from measurements of the migration rate of sand ripples and dune lee fronts at the Nili Patera dune field [ Bridges et al ., ].…”

Section: Rate Of Crater Modificationmentioning

confidence: 99%

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Small crater modification on Meridiani Planum and implications for erosion rates and climate change on Mars

et al. 2014

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A morphometric and morphologic catalog of~100 small craters imaged by the Opportunity rover over the 33.5 km traverse between Eagle and Endeavour craters on Meridiani Planum shows craters in six stages of degradation that range from fresh and blocky to eroded and shallow depressions ringed by planed off rim blocks. The age of each morphologic class from <50-200 ka to~20 Ma has been determined from the size-frequency distribution of craters in the catalog, the retention age of small craters on Meridiani Planum, and the age of the latest phase of ripple migration. The rate of degradation of the craters has been determined from crater depth, rim height, and ejecta removal over the class age. These rates show a rapid decrease from~1 m/Myr for craters <1 Ma to~<0.1 m/Myr for craters 10-20 Ma, which can be explained by topographic diffusion with modeled diffusivities of~10 À6 m 2 /yr. In contrast to these relatively fast, short-term erosion rates, previously estimated average erosion rates on Mars over~100 Myr and 3 Gyr timescales from the Amazonian and Hesperian are of order <0.01 m/Myr, which is 3-4 orders of magnitude slower than typical terrestrial rates. Erosion rates during the Middle-Late Noachian averaged over~250 Myr, and~700 Myr intervals are around 1 m/Myr, comparable to slow terrestrial erosion rates calculated over similar timescales. This argues for a wet climate before~3 Ga in which liquid water was the erosional agent, followed by a dry environment dominated by slow eolian erosion.

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Section: Discussion: Erosion Rate Changes With Timementioning

confidence: 99%

Section: Rate Of Crater Modificationmentioning

confidence: 99%

Small crater modification on Meridiani Planum and implications for erosion rates and climate change on Mars

et al. 2014

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“…Median backweathering rates as a function of crater age (= measurement time interval) for the studied Martian craters, Meteor crater (i.e., Barringer crater) on Earth, the reported terrestrial rock faces given in Figure and Table S1, and the erosion rates reported in Golombek et al [] (as shown in their Figure 25, compiled from data of Malin and Edgett [], McEwen et al [], Golombek et al [], De Haas et al [], Golombek et al [], and Farley et al []). Backweathering rates for Meteor crater were derived with the method applied to the Martian craters, using a LiDAR DEM with 1 m spatial resolution (Figure S12 and Data Set S1; http://www. lpi.usra.edu/publications/books/barringer/crater/guidebook/LiDAR/), the age of Meteor crater is 49±3 ka [ Sutton , ; Nishiizumi et al , ; Phillips et al , ].…”

Section: Discussionmentioning

confidence: 99%

“…Pristine craters are important chronostratigraphic markers for recent exogenic processes acting on the Martian surface [e.g., Schon and Head , ; Johnsson et al , ]. Constraining the timing of these impacts facilitates quantifying rates of the exogenic processes acting upon craters since their formation [e.g., De Haas et al , , ]. Pristine, Late Amazonian aged, craters enable (1) the measurement of relatively recent, Late Amazonian, backweathering rates and (2) the determination of their age because they have well‐defined rays and ejecta on which the size‐frequency distribution of superposed craters can be estimated.…”

Section: Methodsmentioning

confidence: 99%

Recent (Late Amazonian) enhanced backweathering rates on Mars: Paracratering evidence from gully alcoves

2015

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The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. Abstract Mars is believed to have been exposed to low planet-wide weathering and denudation since the Noachian. However, the widespread occurrence of alcoves at the rim of pristine impact craters suggests locally enhanced recent backweathering rates. Here we derive Late Amazonian backweathering rates from the alcoves of 10 young equatorial and midlatitude craters. The enhanced Late Amazonian Martian backweathering rates (10 −4 -10 −1 mm yr −1 ) are approximately 1 order of magnitude higher than previously reported erosion rates and are similar to terrestrial rates inferred from Meteor crater and various Arctic and Alpine rock faces. Alcoves on initially highly fractured and oversteepened crater rims following impact show enhanced backweathering rates that decline over at least 10 1 -10 2 Myr as the crater wall stabilizes. This "paracratering" backweathering decline with time is analogous to the paraglacial effect observed in rock slopes after deglaciation, but the relaxation timescale of 10 1 -10 2 Myr compared to 10 kyr of the Milankovitch-controlled interglacial duration questions whether a paraglacial steady state is reached on Earth. The backweathering rates on the gullied pole-facing alcoves of the studied midlatitude craters are much higher (∼2-60 times) than those on slopes with other azimuths and those in equatorial craters. The enhanced backweathering rates on gullied crater slopes may result from liquid water acting as a catalyst for backweathering. The decrease in backweathering rates over time might explain the similar size of gullies in young (<1 Ma) and much older craters, as alcove growth and sediment supply decrease to low-background rates over time.

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“…This criterion was previously used to prove for certain valleys that they were not formed by seepage erosion (Craddock and Howard, 2002;Lamb et al, 2006). When considering valleys on Mars, the ability of the flow to transport the material should be considered as well as possible weathering rates which may both obscure the former presence of large block or increases erosion (de Haas et al, 2013).…”

Section: Sedimentary Depositsmentioning

confidence: 99%

Valley formation by groundwater seepage, pressurized groundwater outbursts and crater-lake overflow in flume experiments with implications for Mars

Marra

Braat

Baar

et al. 2014

Icarus

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Local late Amazonian boulder breakdown and denudation rate on Mars

Cited by 34 publications

References 49 publications

Small crater modification on Meridiani Planum and implications for erosion rates and climate change on Mars

Small crater modification on Meridiani Planum and implications for erosion rates and climate change on Mars

Recent (Late Amazonian) enhanced backweathering rates on Mars: Paracratering evidence from gully alcoves

Valley formation by groundwater seepage, pressurized groundwater outbursts and crater-lake overflow in flume experiments with implications for Mars

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