Structural uplift and ejecta thickness of lunar mare craters: New insights into the formation of complex crater rims

Krüger, T.; Kenkmann, T.; Hergarten, Stefan

doi:10.1111/maps.12925

Cited by 13 publications

(19 citation statements)

References 38 publications

(143 reference statements)

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“…In this case, modification of the transient crater would cause slumping of material into the crater, resulting in a final crater that is larger than the transient crater (summarized recently, e.g., by Krüger et al. ). Zhu et al.…”

Section: Discussionmentioning

confidence: 98%

“…For complex craters, different relationships to estimate the ratio between final crater radius R final and transient crater radius R have been suggested by different authors (e.g., Croft ; Holsapple ; Krüger et al. ). They all assume that the gravity‐driven enlargement of the transient crater results in a much larger ratio between final crater and transient crater radius in the case of complex crater formation.…”

Section: Theoretical Backgroundmentioning

confidence: 99%

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Effect of target properties and impact velocity on ejection dynamics and ejecta deposition

Luther

Zhu

Collins

et al. 2018

Meteorit & Planetary Scien

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Impact craters are formed by the displacement and ejection of target material. Ejection angles and speeds during the excavation process depend on specific target properties. In order to quantify the influence of the constitutive properties of the target and impact velocity on ejection trajectories, we present the results of a systematic numerical parameter study. We have carried out a suite of numerical simulations of impact scenarios with different coefficients of friction (0.0–1.0), porosities (0–42%), and cohesions (0–150 MPa). Furthermore, simulations with varying pairs of impact velocity (1–20 km s−1) and projectile mass yielding craters of approximately equal volume are examined. We record ejection speed, ejection angle, and the mass of ejected material to determine parameters in scaling relationships, and to calculate the thickness of deposited ejecta by assuming analytical parabolic trajectories under Earth gravity. For the resulting deposits, we parameterize the thickness as a function of radial distance by a power law. We find that strength—that is, the coefficient of friction and target cohesion—has the strongest effect on the distribution of ejecta. In contrast, ejecta thickness as a function of distance is very similar for different target porosities and for varying impact velocities larger than ~6 km s−1. We compare the derived ejecta deposits with observations from natural craters and experiments.

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Section: Discussionmentioning

confidence: 98%

Section: Theoretical Backgroundmentioning

confidence: 99%

Effect of target properties and impact velocity on ejection dynamics and ejecta deposition

Luther

Zhu

Collins

et al. 2018

Meteorit & Planetary Scien

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“…Journal of Geophysical Research: Planets Figure 4. Crater measurements on the ejecta blankets of the 15 initially selected craters in Figure 4 using CraterTools (Kneissl et al, 2011). We conducted crater counting on the relatively smooth regions that lie within the continuous ejecta deposits, excluding obvious secondary crater fields (Michael & Neukum, 2010) and boulder-rich areas (Williams et al, 2014), and the blue polygons show the boundaries of the measurements.…”

Section: 1029/2019je006112mentioning

confidence: 99%

The Provenance of Regolith at the Chang'e‐5 Candidate Landing Region

Xie

Zhang

2020

JGR Planets

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The upcoming lunar Chang'e-5 mission is scheduled to land near Mons Rümker, in northern Oceanus Procellarum, and return samples with masses up to 2 kg from depths up to~2 m. A clear understanding of the regolith components in the candidate landing region is crucial to both the selection of sampling sites and the interpretation of the geological affinities for the returned samples. We quantitatively estimate the abundance of distantly sourced particles (DSPs) in the regolith at the landing region using an updated ballistic sedimentation model. Our results suggest that older units have a higher abundance of DSPs. In the targeted landing area, the total abundance of DSPs on the surface of the regolith varies from approximately 12% to 20%, and most of the DSPs on the surface are ejecta from the Pythagoras (~5%) and/or Aristarchus (~7%) craters. The youngest geological unit, which is located in the easternmost sector of the landing region, possesses the least DSPs in the regolith. Therefore, sampling the eastern unit has a higher potential of revealing both the petrological characteristics and age of the youngest mare basalt, which are fundamentally important to improve both the lunar crater chronology and the understanding of late-stage evolution of the Moon. Our results also indicate that the anorthositic material within the shallow regolith is most likely ejected from the Pythagoras and Aristarchus craters, which could further improve the understanding of lunar geology and chronology.Plain Language Summary Chang'e-5 will be the first lunar sample return mission since the 1976 Luna 24 mission. It will return surface and core samples with masses up to 2 kg from depths up to~2 m from northern Oceanus Procellarum. Most of the returned samples are expected to be lunar regolith. A better understanding of the regolith components in the candidate landing region is therefore helpful to both select sampling sites and interpret the samples that will be returned in the future. Here, we estimate the abundance of distantly sourced particles (DSPs) in the regolith within the proposed landing region. We find that older units are more enriched in DSPs, and the total surface abundance of DSPs varies from approximately 12% to 20%. Most DSPs on the surface are ejecta from the Pythagoras (~5%) and/or Aristarchus (~7%) craters. Our results support that the youngest mare unit is most suitable for sample return because of the low abundance of DSPs. Furthermore, core samples from this unit contain not only local basaltic materials and the several major sources of distant ejecta in the regolith but also both pristine highland anorthosites and pyroclastic deposits.

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“…well-constrained measurement of this parameter is important for correctly applying scaling laws (e.g., Holsapple, 1993;Holsapple & Housen, 2007), and calculating the transient crater diameter, ejecta thicknesses, and for comparison with numerical models of impact craters (e.g., Collins et al, 2012;Croft, 1985;Krüger et al, 2017;McGetchin et al, 1973;Wünnemann et al, 2011).…”

Section: Introductionmentioning

confidence: 99%

“…This parameter is used to define the simple‐to‐complex transition diameter or the degradational state of craters (e.g., Kalynn et al, ; Malin & Dzurisin, ; Melosh, ; Pike, , , ; Robbins & Hynek, ; Robbins et al, ; Wood & Anderson, ; Wünnemann & Ivanov, ). A well‐constrained measurement of this parameter is important for correctly applying scaling laws (e.g., Holsapple, ; Holsapple & Housen, ), and calculating the transient crater diameter, ejecta thicknesses, and for comparison with numerical models of impact craters (e.g., Collins et al, ; Croft, ; Krüger et al, ; McGetchin et al, ; Wünnemann et al, ).…”

Section: Introductionmentioning

confidence: 99%

Deriving Morphometric Parameters and the Simple‐to‐Complex Transition Diameter From a High‐Resolution, Global Database of Fresh Lunar Impact Craters (D ≥ ~ 3 km)

2018

Self Cite

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We compiled a high‐resolution, global lunar impact crater database composed of 5,505 pristine craters ≥ ~3 km. This database contains detailed morphometric data, and their trends are examined with best‐fit power‐laws. We compared several different functions for simple, transitional, and complex craters to report one best‐fit representation. We integrated transitional craters into these fits as an independent crater class. Transitional craters are in a transitional state, between simple and complex craters. They are devoid of a central uplift and terraces but show wall slumping and a flat floor. In regard to depth‐diameter relationships, simple craters exhibit similar scaling all over the Moon, whereas larger craters are different in highland and mare regions. In the present work, we sought the best representation of the simple‐to‐complex transition diameter. The intersection of simple power‐law fits for simple and complex crater populations is shown to be a poor representation of the transition diameter. We used a misclassification method for finding transition diameters. This process reveals a transition from simple to transitional craters at diameters of ~17 km (highland) and ~14 km (mare). Transitional morphology is replaced by complex morphology at diameters of ~ 28 km (highland) and ~ 24 km (mare). The lower transition diameters of mare craters are attributed primarily to the layered mare basalts, which enables an earlier onset of crater modification. We also analyzed the relationship between aspect ratio and depth‐diameter ratio of simple craters: Simple craters with ε ≥ 1.1 are significantly shallower in depth/diameter plots than craters with ε < 1.1.

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Structural uplift and ejecta thickness of lunar mare craters: New insights into the formation of complex crater rims

Cited by 13 publications

References 38 publications

Effect of target properties and impact velocity on ejection dynamics and ejecta deposition

Effect of target properties and impact velocity on ejection dynamics and ejecta deposition

The Provenance of Regolith at the Chang'e‐5 Candidate Landing Region

Deriving Morphometric Parameters and the Simple‐to‐Complex Transition Diameter From a High‐Resolution, Global Database of Fresh Lunar Impact Craters (D ≥ ~ 3 km)

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