Lunar crater morphology and relative age determination of lunar geologic units - Part 1, Classification; Part 2, Applications

Pohn, H. A.; Offield, Terry W.

doi:10.3133/ofr69209

Cited by 48 publications

(56 citation statements)

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“…9) compared to the range of impact craters between 20 and 720 km. This is in good agreement with Pohn and Offield (1970) and Öhman (2009) who stated that PICs have a tendency to be most common in the size range of mid-sized complex craters. A similar result was found on the Moon, on Mars, and Venus, therefore it can be interpreted as a general "rule".…”

Section: Distribution Of Pics On the Surfacesupporting

confidence: 92%

“…The shape of a polygonal impact crater is established during the crater formation and that the subsequent crater degradation does not have a significant effect on it (Pohn and Offield, 1970;Öhman et al, 2006). There exist three models of formation, two first formulated by Eppler et al (1983) and a third one by Öhman et al (2008).…”

Section: Formation Of Polygonal Impact Craters (Pics)mentioning

confidence: 99%

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Polygonal impact craters on mercury

Weihs

Leitner

Firneis

2015

Planetary and Space Science

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Section: Distribution Of Pics On the Surfacesupporting

confidence: 92%

Section: Formation Of Polygonal Impact Craters (Pics)mentioning

confidence: 99%

Polygonal impact craters on mercury

Weihs

Leitner

Firneis

2015

Planetary and Space Science

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“…Arthur, Agnieray, Horvath, Wood, & Chapman, 1963;Baker & Head, 2013;Cintala, Head, & Mutch, 1976;Leake, 1982;McCauley, Guest, Schaber, Trask, & Greeley, 1981;Pohn & Offield, 1970;Spudis & Guest, 1988;Wood, 1979;Wood & Anderson, 1978;Wood, Head, & Cintala, 1977). The M10 geological mapping project used a crater classification system with five classes of craters (McCauley et al, 1981): M10/C1 are the oldest and most degraded craters, while M10/C5 are the youngest and least degraded craters.…”

Section: Crater Materials Classificationmentioning

confidence: 99%

Geology of the Victoria quadrangle (H02), Mercury

et al. 2016

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Mercury's quadrangle H02 'Victoria' is located in the planet's northern hemisphere and lies between latitudes 22.5°N and 65°N, and between longitudes 270°E and 360°E. This quadrangle covers 6.5% of the planet's surface with a total area of almost 5 million km 2 . Our 1:3,000,000-scale geologic map of the quadrangle was produced by photo-interpretation of remotely sensed orbital images captured by the MESSENGER spacecraft. Geologic contacts were drawn between 1:300,000 and 1:600,000 mapping scale and constitute the boundaries of intercrater, intermediate and smooth plains units; in addition, three morpho-stratigraphic classes of craters larger than 20 km were mapped. The geologic map reveals that this area is dominated by Intercrater Plains encompassing some almost-coeval, probably younger, Intermediate Plains patches and interrupted to the north-west, north-east and east by the Calorian Northern Smooth Plains. This map represents the first complete geologic survey of the Victoria quadrangle at this scale, and an improvement of the existing 1:5,000,000 Mariner 10-based map, which covers only 36% of the quadrangle. ARTICLE HISTORY

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“…Features used by previous investigators to recognize morphologic modification of craters with time include crater rim crispness and the presence or absence of continuous ejecta deposits and secondary impact features [e.g., Pohn and Offield, 1970;Arthur, 1963Arthur, , 1974Pike, 1974]. Terraced interior walls, central peaks or rings, and crater floor morphology have been interpreted as products of postimpact mass movements, such as slumping or landsliding from crater walls, or isostatic rebound of crater floors [e.g., Pike, 1974;Head, 1975].…”

Section: Morphologic Indicatorsmentioning

confidence: 99%

Landform degradation on Mercury, the Moon, and Mars: Evidence from crater depth/diameter relationships

Malin

Dzurisin

1977

J. Geophys. Res.

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Morphologic classification of craters and quantitative measurements of crater depth as a function of diameter are used to investigate the relative degradational histories of Mercury, the moon, and Mars. Martian craters exhibit considerable depth variation and are generally shallower than their lunar or mercurian counterparts. On Mercury and the moon, visually fresh and degraded craters on smooth plains show no significant depth degradation except that attributed to lava flooding or local inundation by ejecta from large impacts. More heavily cratered regions on both planets display a large range of both visual and depth degradation, suggesting that most landform modification occurred before the final phase of formation of the oldest smooth plains on both planets. Depth/ diameter data presented here are discussed as they relate to two early history scenarios. One scenario based on cratering and the ballistic tqrnsport of material has been suggested for Mercury, the moon, and Mars by several authors. Owing to discrepancies between this ballistic scenario and observations of crater densities and morphologies, we suggest that landforms on all these bodies also record nonballistic degradation associated with the formation of intercrater plains. Whichever scenario is applied, early, intense, bombardment-associated degradation appears to be a common element in the histories of the terrestrial planets.

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Lunar crater morphology and relative age determination of lunar geologic units - Part 1, Classification; Part 2, Applications

Cited by 48 publications

References 0 publications

Polygonal impact craters on mercury

Polygonal impact craters on mercury

Geology of the Victoria quadrangle (H02), Mercury

Landform degradation on Mercury, the Moon, and Mars: Evidence from crater depth/diameter relationships

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