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

Krüger, T.; Bogert, C. H. van der; Hiesinger, H.

doi:10.1016/j.icarus.2016.02.018

Cited by 35 publications

(15 citation statements)

References 43 publications

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“…Assuming convection took place in an impact melt sheet filling the Hellas basin up to the approximate elevation of the honeycomb terrain, the preservation, i.e., “recording,” of such upwelling structures would be the next crucial step. On the Moon, occurrences of relatively fresh impact melt in environments lacking decisive subsequent tectonic deformation can indeed contain “fossilized” fluid movement that is now represented as solidified surface morphology [e.g., Bray et al ., ; Krüger et al ., ]. However, no cell‐like, periodic patterns reminiscent of frozen convection have been identified, neither in such fresh melt pools [ Bray et al ., ] nor in the SIC in Canada [ Zieg and Marsh , ] or on the floors of other comparably sized basins in the solar system (e.g., South Pole‐Aitken, Caloris, Imbrium, Isidis, and Argyre) [e.g., Andrews‐Hanna and Zuber , ].…”

Section: Discussionmentioning

confidence: 99%

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The honeycomb terrain on the Hellas basin floor, Mars: A case for salt or ice diapirism

et al. 2016

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We present quantitative plausibility studies of potential formation mechanisms for the “honeycomb” terrain on the northwestern Hellas basin floor. The honeycomb terrain is a unique landscape of ~10.5 × 5 km wide, mostly cell‐shaped depressions that are arranged in a regular, dense pattern covering ~36,000 km2. We argue against the honeycombs being (peri)glacial landforms (till rings, iceberg imprints, and thermokarst) or the result of igneous diapirism, as terrestrial analogs do not reproduce their key characteristics. Fossilized impact melt convection cells also appear to be an unsuitable interpretation, as melt solidification should not permit such structures to be retained. We present arguments in favor of salt or ice diapirism as honeycomb formation models. Honeycomb‐sized diapirs could be formed by a ~2 km thick salt layer (~72,000 km3 for the entire honeycomb terrain), which might have been derived from the highlands north of Hellas Planitia—an area of abundant chloride signatures and intense snowfall according to ancient Mars climate models. Nearby volcanic activity ~3.8 Ga ago potentially enabled recurring phases of (probably salty) meltwater runoff (as indicated by meandering channels) and might therefore have enabled evaporite deposition in the Hellas basin. Being twice as buoyant as salt, water ice would require an only ~1 km thick layer (i.e., ~36,000 km3) to form honeycomb‐sized diapirs, which would be in agreement with a likely ~2 km thick ice stability zone beneath the Hellas basin floor. However, it would remain an open question as to why we find only one such ice diapir landscape on Mars.

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Section: Discussionmentioning

confidence: 99%

“…[]; [10] Bray et al [] and Krüger et al . []; [11] e.g., Ramsay []; [12] e.g., Diegel et al . []; [13] Schenk and Jackson []; [14] Manneville []; [15] Blight et al .…”

Section: Discussionmentioning

confidence: 99%

The honeycomb terrain on the Hellas basin floor, Mars: A case for salt or ice diapirism

et al. 2016

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“…Outside the rim, this unit corresponds to the ejecta blanket and to surfaces modified by scouring and secondary impacts. Ponded deposits have the same morphologies as material interpreted to be impact melt on the Moon and Vesta (e.g., Krueger et al, 2016;Williams et al, 2014;Neish et al, 2014;Denevi et al, 2012;Plescia and Cintala, 2012;Bray et al, 2010 ) and might share the same origin (e.g., Krohn et al, 2016 ). Buczkowski et al (2016) identify a similarity between the crater material located north of unnamed crater A (28 °E-69 °N) ( Fig.…”

Section: Map Unit Descriptionmentioning

confidence: 96%

Geology of Ceres’ North Pole quadrangle with Dawn FC imaging data

Ruesch

McFadden

Williams

et al. 2018

Icarus

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The Dawn Framing Camera repeatedly imaged Ceres' North Pole quadrangle (Ac-1 Asari, latitudes > 66 °N) at a resolution of ∼35 m/pixel through a panchromatic filter, enabling the derivation of a digital terrain model (DTM) and an ortho-rectified mosaic. Using this dataset, a photo-geologic map and stratigraphy, complemented with absolute model ages of impact craters, were produced. We identified the following key surface features: an ancient 4.5 km high isolated dome with a non-impact origin; recent lobate materials on crater interiors possibly formed as high-speed flows of collapsed rim material; and recent bright areas in permanently shadowed regions (PSRs), which we interpret as ice accumulation mostly by infall of exogenic material. Crater morphologies and dimensions do not differ from those in other quadrangles, suggesting the widespread influence of a rheologically weak target during the crater formation process. There is a paucity of lobate materials associated with impact cratering, in contrast to previous identifications with lower spatial resolution imagery.

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“…LROC and Diviner have yielded a wealth of detailed data for the surface of the Moon. Among other scientific objectives, these data allowed refining model ages for surface features on the Moon (e.g., Hiesinger et al 2012;Kirchoff et al 2013;Kramer et al 2013;Braden et al 2014;Ashley et al 2016;Kr€ uger et al 2016;Shirley et al 2016;Clark et al 2017;Orgel et al 2018; Van der Bogert et al 2017;Zanetti et al 2017;Povilaitis et al 2018), unraveling lithologic variations associated with impact craters (Bray et al 2010(Bray et al , 2018Spudis et al 2011;Ashley et al 2012;Denevi et al 2012;Plescia and Cintala 2012;Plescia and Spudis 2014;Stopar et al 2014;Wagner and Robinson 2014;Meyer et al 2016;Robinson et al 2016;Spudis and Sliz 2017), and revealing young impact craters based on characteristics of the albedo and surface roughness associated with their ejecta (Bandfield et al 2011;Cahill et al 2014;Ghent et al 2014Ghent et al , 2016Greenhagen et al 2016;Williams et al 2016;Hayne et al 2017). However, linking LROC and Diviner data to lunar meteorites has not been attempted so far.…”

Section: Introductionmentioning

confidence: 99%

Petrogenesis of lunar impact melt rock meteorite Oued Awlitis 001

Wittmann

Korotev

Jolliff

et al. 2018

Meteorit & Planetary Scien

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Oued Awlitis 001 is a highly feldspathic, moderately equilibrated, clast‐rich, poikilitic impact melt rock lunar meteorite that was recovered in 2014. Its poikilitic texture formed due to moderately slow cooling, which judging from textures of rocks in melt sheets of terrestrial impact structures, is observed in impact melt volumes at least 100 m thick. Such coherent impact melt volumes occur in lunar craters larger than ~50 km in diameter. The composition of Oued Awlitis 001 points toward a crustal origin distant from incompatible‐element‐rich regions. Comparison of the bulk composition of Oued Awlitis 001 with Lunar Prospector 5° γ‐ray spectrometer data indicates a limited region of matches on the lunar farside. After its initial formation in an impact crater larger than ~50 km in diameter, Oued Awlitis 001 was excavated from a depth greater than ~50 m. The cosmogenic nuclide inventory of Oued Awlitis 001 records ejection from the Moon 0.3 Ma ago from a depth of at least 4 m and little mass loss due to ablation during its passage through Earth's atmosphere. The terrestrial residence time must have been very short, probably less than a few hundred years; its exact determination was precluded by a high concentration of solar cosmic ray‐produced 14C. If the impact that excavated Oued Awlitis 001 also launched it, this event likely produced an impact crater >10 km in diameter. Using petrologic constraints and Lunar Reconnaissance Orbiter Camera and Diviner data, we test Giordano Bruno and Pierazzo as possible launch craters for Oued Awlitis 001.

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

Cited by 35 publications

References 43 publications

The honeycomb terrain on the Hellas basin floor, Mars: A case for salt or ice diapirism

The honeycomb terrain on the Hellas basin floor, Mars: A case for salt or ice diapirism

Geology of Ceres’ North Pole quadrangle with Dawn FC imaging data

Petrogenesis of lunar impact melt rock meteorite Oued Awlitis 001

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