Origin of discrepancies between crater size-frequency distributions of coeval lunar geologic units via target property contrasts

Bogert, C. H. van der; Hiesinger, H.; Dundas, C. M.; Krüger, T.; McEwen, A. S.; Zanetti, M.; Robinson, M. S.

doi:10.1016/j.icarus.2016.11.040

Cited by 55 publications

(45 citation statements)

References 59 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Similar discrepancies between the model ages of the ejecta blanket and melt deposits were observed at other Copernican craters (e.g., van der Bogert et al, 2010;Ashley et al, 2012;Zanetti et al, 2016;van der Bogert et al, 2016 ). Hiesinger et al (2012), as well as van der Bogert et al (2010van der Bogert et al ( , 2013van der Bogert et al ( , 2016 , discuss potential sources for the differences. Self-secondary cratering might cause an excess of craters on the ejecta relative to melt deposits ( Shoemaker et al, 1968;Plescia et al, 2010;Plescia and Robinson, 2011;Zanetti et al, 2014Zanetti et al, , 2016.…”

Section: Absolute Model Agessupporting

confidence: 58%

“…Self-secondary cratering might cause an excess of craters on the ejecta relative to melt deposits ( Shoemaker et al, 1968;Plescia et al, 2010;Plescia and Robinson, 2011;Zanetti et al, 2014Zanetti et al, , 2016. Alternatively, different target properties could cause final crater diameters to be smaller on melt versus ejecta ( Schultz et al, 1977;Dundas et al, 2010 ;van der Bogert et al, 2016 ). As a result, Hiesinger et al (2012) used the ages derived from the ejecta blankets of Tycho, Copernicus, and North Ray to revisit the lunar chronology, because ejecta blanket count areas were used in the initial calibration of the chronology.…”

Section: Absolute Model Agesmentioning

confidence: 99%

See 1 more Smart Citation

Geomorphologic mapping of the lunar crater Tycho and its impact melt deposits

Krüger

Bogert

Hiesinger

2016

Icarus

Self Cite

View full text Add to dashboard Cite

Section: Absolute Model Agessupporting

confidence: 58%

Section: Absolute Model Agesmentioning

confidence: 99%

Geomorphologic mapping of the lunar crater Tycho and its impact melt deposits

Krüger

Bogert

Hiesinger

2016

Icarus

Self Cite

View full text Add to dashboard Cite

“…North is toward the top. The base images are obtained by LROC NAC trajectory), as normal ejecta deposits have larger crater densities (e.g., van der Bogert et al 2010;Zanetti et al 2017). For example, Fig.…”

Section: Self-secondaries On the Moonmentioning

confidence: 99%

“…4) and their dominance in small crater populations on the continuous ejecta deposits of newly formed impact craters (e.g., the Hokusai case on Mercury), however, there are debates about whether or not self-secondaries are needed to explain the observed crater density differences on Copernican-aged lunar craters. Contemporaneous with the return of the self-secondaries scenario , the long-ignored but poorly understood effect of target properties on the SFD of small impact craters were interpreted to be the cause for the larger crater density on normal ejecta deposits than melt pools (e.g., van der Bogert et al 2010). According to this interpretation, different target properties (e.g., density, cohesion, porosity) can cause up to 2 times differences in crater rim-to-rim diameters for same-energy impactors, so that small craters formed on melt pools and normal ejecta deposits have both different SFD and densities .…”

Section: Formation Mechanism Of Self-secondaries On the Moon And Terrmentioning

confidence: 99%

“…Plescia and Spudis (2014) believed that the irregularly shaped small craters on the melt pools are self-secondaries that were formed on the still-molten melt pools. However, the target property difference scenario regarded melt pools as competent rocks that have much larger cohesion and smaller porosity than normal ejecta (Williams and Pathare 2015;van der Bogert et al 2017). Nevertheless, even assuming that craters formed on melt pools are 2 times smaller than those on normal ejecta deposits assuming same impactors, the large crater density difference still exists (Xiao 2016;Zanetti et al 2017).…”

Section: Formation Mechanism Of Self-secondaries On the Moon And Terrmentioning

confidence: 99%

See 1 more Smart Citation

On the importance of self-secondaries

Xiao

2018

Geosci. Lett.

View full text Add to dashboard Cite

Self-secondaries are secondary craters that are formed on both the continuous ejecta deposits and interior of the parent crater. The possible existence of self-secondaries was proposed in the late 1960s, but their identity, formation mechanism, and importance were not revisited until the new generation of high-resolution images for the Moon have recently became available. Possible self-secondary crater populations have now been recognized not only on the Moon, but also on Mercury, Mars, 1Ceres, 4Vesta, and satellites of the ice giants. On the Moon and terrestrial planets, fragments that form self-secondaries are launched with high ejection angles via spallation during the early cratering process, so that self-secondaries can be formed both within the crater and on the continuous ejecta deposits at the end of the cratering process. Self-secondaries potentially possess profound effects on the widely used agedetermination technique using crater statistics in planetary geology, because (1) self-secondaries cause nonuniform crater density across the continuous ejecta deposits, which cannot be solely explained by the effect of different target properties on crater size-frequency distributions; (2) crater chronologies for both the Moon and the other terrestrial bodies are largely based on crater counts on the continuous ejecta deposits of several young lunar craters. The effect of self-secondaries on crater chronology can be well addressed after the spatial distribution, size-frequency distribution, and density evolution of self-secondaries are resolved.

show abstract

Amazonian fluvial outflow channels in Jovis Tholus region, Mars

Vijayan

Sinha

2017

JGR Planets

View full text Add to dashboard Cite

Outflow channels are prevalent on the surface of Mars, and they are one of the strongest lines of evidence for fluvial activity. The purported presence of some of the channel networks on the Amazonian surface provides evidence for recent surficial fluvial activity. We describe morphological evidence collectively diagnostic of fluvial origin for the channels located northwest (NW) of Jovis Tholus, within the Tharsis volcanic province. The fluvial relationships are deciphered from (1) morphological analysis of catastrophic effusion associated with the graben system superposed over the NW portion of an unnamed crater ejecta (19.85°N, 118.03°W) and (2) crater‐size frequency distributions of unnamed crater ejecta revealing the tentative period of the fluvial activity. Channels, streamlined/curvilinear islands, terraces, divide crossing, crossover channels, networks of braided‐like channels, and eroded ejecta are collectively suggestive of fluvial outflow that emanated from the graben. Chronological analysis revealed that the unnamed crater formed at ~3.4 Ga. Subsequently, the NW part of crater ejecta was incised by a channel network originated from the graben. Furthermore, we infer that the current channel floor has undergone volcanic and aeolian resurfacing to some extent, and the estimated modeled resurfaced channel age is ~0.2–0.5 Ga. This reveals that the fluvial activity possibly occurred after the crater formation, but before channel floor resurfacing, which is during Early to Middle Amazonian. Nevertheless, the potential source for the channel formation likely persisted under this region since the pre‐Amazonian epoch. The suite of these fluvial features inferred within the Jovis Tholus region outflow channel system thus adds one another evidence for Amazonian fluvial activity.

show abstract

Origin of discrepancies between crater size-frequency distributions of coeval lunar geologic units via target property contrasts

Cited by 55 publications

References 59 publications

Geomorphologic mapping of the lunar crater Tycho and its impact melt deposits

Geomorphologic mapping of the lunar crater Tycho and its impact melt deposits

On the importance of self-secondaries

Amazonian fluvial outflow channels in Jovis Tholus region, Mars

Contact Info

Product

Resources

About