The geology of the terrestrial planets

Carr, M. H.

doi:10.1029/rg021i002p00160

Cited by 24 publications

(28 citation statements)

References 448 publications

(640 reference statements)

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“…Furthermore, the topography falls from the eastern boundary at about 8 km above the Mars reference datum to near 0 km at the western boundary. Viking images of the ensemble of regions making up Stealth have been studied by many investigators including Scott & Tanaka (1982), Cart (1984), and Schultz & Lutz (1988). The geological map of Scott Tanaka (1986) shows that much of the eastern and northern parts of Stealth lies in the upper and middle Medusae Fossae units.…”

Section: Stealthmentioning

confidence: 99%

Radar Investigation of Mars, Mercury, and Titan

Muhleman¹,

Grossman²,

Butler³

1995

Annu. Rev. Earth Planet. Sci.

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Section: Stealthmentioning

confidence: 99%

Radar Investigation of Mars, Mercury, and Titan

Muhleman¹,

Grossman²,

Butler³

1995

Annu. Rev. Earth Planet. Sci.

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“…Geologic mapping is an investigative process that seeks to understand the evolution of planetary surfaces (Carr et al, , 1984Greeley and Carr, 1976;Wilhelms, 1990;Hansen, 2000;Tanaka et al, 2010). Geologic maps are thus tools that show the stratigraphic sequence of map units defined by geologic processes.…”

Section: Introductionmentioning

confidence: 99%

The chronostratigraphy of protoplanet Vesta

Williams

Jaumann

McSween

et al. 2014

Icarus

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a b s t r a c tIn this paper we present a time-stratigraphic scheme and geologic time scale for the protoplanet Vesta, based on global geologic mapping and other analyses of NASA Dawn spacecraft data, complemented by insights gained from laboratory studies of howardite-eucrite-diogenite (HED) meteorites and geophysical modeling. On the basis of prominent impact structures and their associated deposits, we propose a time scale for Vesta that consists of four geologic time periods: Pre-Veneneian, Veneneian, Rheasilvian, and Marcian. The Pre-Veneneian Period covers the time from the formation of Vesta up to the Veneneia impact event, from 4.6 Ga to >2.1 Ga (using the asteroid flux-derived chronology system) or from 4.6 Ga to 3.7 Ga (under the lunar-derived chronology system). The Veneneian Period covers the time span between the Veneneia and Rheasilvia impact events, from >2.1 to 1 Ga (asteroid flux-derived chronology) or from 3.7 to 3.5 Ga (lunar-derived chronology), respectively. The Rheasilvian Period covers the time span between the Rheasilvia and Marcia impact events, and the Marcian Period covers the time between the Marcia impact event until the present. The age of the Marcia impact is still uncertain, but our current best estimates from crater counts of the ejecta blanket suggest an age between $120 and 390 Ma, depending upon choice of chronology system used. Regardless, the Marcia impact represents the youngest major geologic event on Vesta. Our proposed four-period geologic time scale for Vesta is, to a first order, comparable to those developed for other airless terrestrial bodies.

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“…Close to the shoreline, and especially near the outflow channels, smaller marine-target craters are probably covered by huge amounts of fluvial and colluvial sediments, and features like resurge gullies at bigger craters may be hard to recognize. Large quantities of material have apparently been transported to the northern plains by repeated catastrophic floods (Baker et al 1991;Dohm et al 2001a, b;Fairén et al 2003), and eolian deposition has persisted for much of the suitable areas for potential marinetarget craters (Carr et al 1984). Furthermore, impact structures can act as efficient sediment traps (Lindström et al 1994;Hartmann and Neukum 2001).…”

Section: Exposure and Examples Of Possible Marine-target Cratersmentioning

confidence: 99%

Marine‐target craters on Mars? An assessment study

Ormö

Dohm

Ferris

et al. 2004

Meteorit & Planetary Scien

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Marine-target craters on Mars? An assessment studyAbstract-Observations of impact craters on Earth show that a water column at the target strongly influences lithology and morphology of the resultant crater. The degree of influence varies with the target water depth and impactor diameter. Morphological features detectable in satellite imagery include a concentric shape with an inner crater inset within a shallower outer crater, which is cut by gullies excavated by the resurge of water. In this study, we show that if oceans, large seas, and lakes existed on Mars for periods of time, marine-target craters must have formed. We make an assessment of the minimum and maximum amounts of such craters based on published data on water depths, extent, and duration of putative oceans within "contacts 1 and 2," cratering rate during the different oceanic phases, and computer modeling of minimum impactor diameters required to form longlasting craters in the seafloor of the oceans. We also discuss the influence of erosion and sedimentation on the preservation and exposure of the craters.

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The geology of the terrestrial planets

Cited by 24 publications

References 448 publications

Radar Investigation of Mars, Mercury, and Titan

Radar Investigation of Mars, Mercury, and Titan

The chronostratigraphy of protoplanet Vesta

Marine‐target craters on Mars? An assessment study

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