Chicxulub impact ejecta from Albion Island, Belize

Pope, Kevin; Ocampo, A.; Fischer, Alfred G.; Álvarez, Walter; Fouke, Bruce W.; Webster, C.; Vega, Francisco J.; Smit, Jan; Fritsche, A. Eugene; Claeys, Philippe

doi:10.1016/s0012-821x(99)00123-5

Cited by 64 publications

(83 citation statements)

References 23 publications

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“…The outer portion of the continuous ejecta blanket has been termed the Albion Formation and comprises a basal spheroid bed and an upper diamictite bed (e.g., Pope et al 1999). Unfortunately, the lack of exposure and drill cores does not allow the exact relationship of the innermost proximal impactites and the Albion Formation to be constrained.…”

Section: Chicxulub Impact Structurementioning

confidence: 99%

Effect of volatiles and target lithology on the generation and emplacement of impact crater fill and ejecta deposits on Mars

Osinski

2006

Meteorit & Planetary Scien

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Effect of volatiles and target lithology on the generation and emplacement of impact crater fill and ejecta deposits on MarsAbstract-Impact cratering is an important geological process on Mars and the nature of Martian impact craters may provide important information as to the volatile content of the Martian crust. Terrestrial impact structures currently provide the only ground-truth data as to the role of volatiles and an atmosphere on the impact-cratering process. Recent advancements, based on studies of several well-preserved terrestrial craters, have been made regarding the role and effect of volatiles on the impact-cratering process. Combined field and laboratory studies reveal that impact melting is much more common in volatile-rich targets than previously thought, so impact-melt rocks, melt-bearing breccias, and glasses should be common on Mars. Consideration of the terrestrial impact-cratering record suggests that it is the presence or absence of subsurface volatiles and not the presence of an atmosphere that largely controls ejecta emplacement on Mars. Furthermore, recent studies at the Haughton and Ries impact structures reveal that there are two discrete episodes of ejecta deposition during the formation of complex impact craters that provide a mechanism for generating multiple layers of ejecta. It is apparent that the relative abundance of volatiles in the near-surface region outside a transient cavity and in the target rocks within the transient cavity play a key role in controlling the amount of fluidization of Martian ejecta deposits. This study shows the value of using terrestrial analogues, in addition to observational data from robotic orbiters and landers, laboratory experiments, and numerical modeling to explore the Martian impact-cratering record.

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Section: Chicxulub Impact Structurementioning

confidence: 99%

Effect of volatiles and target lithology on the generation and emplacement of impact crater fill and ejecta deposits on Mars

Osinski

2006

Meteorit & Planetary Scien

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“…Before this end stage, the main body of the flow loses energy via the frictional interaction between the clasts within the flow. In fact, gouges, grooves, striae, and polished surfaces can be found on ejecta fragments associated with both the Chicxulub structure (Pope et al 1999) and the Ries impact crater (Chao 1976). These examples of high strain rate deformation and frictional melting are analogous to low velocity, low shock oblique impacts between asteroids.…”

Section: Geologic Setting Of Low Shock High Strain Rate Deformationmentioning

confidence: 99%

Impact‐induced frictional melting in ordinary chondrites: A mechanism for deformation, darkening, and vein formation

Bogert

Schultz

Spray

2003

Meteorit & Planetary Scien

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Abstract-High speed friction experiments have been performed on the ordinary chondrites El Hammami (H5, S2) and Sahara 97001 (L6, S3) using an axial friction-welding apparatus. Each sample was subjected to a strain rate of 10 3 to 10 4 s -1 , which generated 250 to 500 mm-deep darkened zones on each sample cube. Thin section analyses reveal that the darkened areas are composed of silicate glass and mineral fragments intermingled with dispersed submicron-size FeNi and FeS blebs.Fracturing of mineral grains and the formation of tiny metallic veins define the extent of deformation beyond the darkened shear zone. These features are not present in the original meteorites. The shear zones and tiny veins are quite similar to certain vein systems seen in naturally deformed ordinary chondrites. The experiments show that shock deformation is not required for the formation of melt veins and darkening in ordinary chondrites. Therefore, the presence of melt veins and darkening does not imply that an ordinary chondrite has undergone severe shock deformation. In fact, high strain rate deformation and frictional melting are especially important for the formation of veins at low shock pressures.

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“…The best example are remnants of distal ejecta from Chicxulub crater (Pope et al 1999;King & Petruny 2003b) combined with the extended cover formed by tsunami waves and submarine avalanches caused by the impact. It is possible that several unique accumulative landforms (debris-flow lobes) may be produced by impact onto the coastal plain or adjacent shelf.…”

Section: Topographic Featuresmentioning

confidence: 99%

Morphological, structural and lithological records of terrestrial impacts: an overview

Масайтис¹

2005

Australian Journal of Earth Sciences

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Chicxulub impact ejecta from Albion Island, Belize

Cited by 64 publications

References 23 publications

Effect of volatiles and target lithology on the generation and emplacement of impact crater fill and ejecta deposits on Mars

Effect of volatiles and target lithology on the generation and emplacement of impact crater fill and ejecta deposits on Mars

Impact‐induced frictional melting in ordinary chondrites: A mechanism for deformation, darkening, and vein formation

Morphological, structural and lithological records of terrestrial impacts: an overview

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