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• W63144865 abstract "Jet Propulsion Laboratory, California Institute ofTechnology, 4800 Oak Grove Drive, Pasadena, CA 91109, aocampo@hq.nasa.gov.Introduction: The relative importance of crustalvolatiles and atmospheres in the emplacement of ejectablankets forms the central part of the debate on theorigin of fluidized ejecta blankets on Mars. Onehypothesis is that fluidized ejecta are a product ofvolatiles (most likely water) in the Martian crust,which when mixed with the solid ejecta caused it toflow like a terrestrial debris flow [1]. Anotherhypothesis is that on planets with atmospheres much ofthe fine-grained ejecta is winnowed out of the ejectacurtain by atmospheric drag, thus producing aturbulent cloud of debris that flows with fluid-likeproperties [2]. The existence of fluidized ejectablankets on Mars is used in arguments for abundantwater in the Martian subsurface [1]. If atmosphericeffects alone can produce these fluidized features, thenthis argument is weakened. If the atmosphere isresponsible for the formation of fluidized ejectablankets, then these features on Mars may provideinformation on past atmospheric conditions [2].In this paper we examine the evidence for fluidizedejecta emplacement by the Chicxulub impact in theYucatan Peninsula of Mexico. Target rocks atChicxulub were rich in volatiles, including water.Earth has a thick atmosphere and therefore ejectaemplacement, especially in the outer parts of the ejectablanket, was affected by atmospheric drag. TheChicxulub impact had conditions that match bothhypotheses for the formation of fluidized ejectablankets, therefore its ejecta blanket may provideinsights into ejecta fluidization mechanisms.Extent and Thickness of the Chicxulub EjectaBlanket: The Chicxulub ejecta blanket has been coredclose to the rim of the crater where the maximumthickness is about 500 m [3]. The only knownexposures of the ejecta blanket come from the AlbionFormation, which is exposed 360 km from the centerof Chicxulub on Albion Island in northern Belize [4],and in recently discovered outcrops directly across theMexican border in Quintana Roo. The maximumobserved thickness of these deposits is 16 m, but mayhave been more. Geological reconnaissance furthersouth in Belize has not located additional exposuresand it appears that the ejecta on Albion Island lie nearthe outer edge of the continuous ejecta blanket.These geological data indicate that the continuousejecta blanket of the Chicxulub crater extends notmuch more than 360 km from the center of impact.Recent geophysical studies place the final Chicxulubcrater diameter at about 200 km, with a transient craterdiameter of 100 km [5]. Ejecta blanket scalingrelationships have been developed for the moon andare widely applicable to other terrestrial planets forcraters up to 436 km in diameter [6]. Scalingrelationships [7] predict that the Chicxulub continuousejecta blanket should extend about 185-288 km,considerably less than the 364 km noted. McGetchin etal. developed a semi-empirical scaling relationship forejecta thickness of large craters based in part on datafrom lunar craters [8]. When this scaling is applied tothe Chicxulub continuous ejecta blanket, it predictsthicknesses about an order of magnitude less thanobserved.Composition of the Chicxulub Ejecta Blanket:Recent studies of the Albion Formation demonstratethat the Chicxulub continuous ejecta blanket iscomposed of multiple flows of debris [4]. Foliation andbasal shear planes between some flows indicatelaminar flow regimes. Lack of these features and ofsize grading in other flows suggests turbulent flow.Some outcrops produced evidence of alternatinglaminar and turbulent flow, typical of distal pyroclasticflows where loss of volatiles (deflation) causes a shiftfrom turbulent to laminar flow.The basal one to two meters of the AlbionFormation (spheroid bed) is composed of up to fourflows containing 10-30% carbonate accretionarylapilli. The lapilli range is size from 1-30 mm andmany have angular cores of dolomite and rarely alteredglass. Altered glass spheroids are abundant in the basalflow. The upper 15 m of the Albion Formation(diamictite bed) contains large carbonate blocks andabout 10% altered glass supported in a dolomite andcalcite silt matrix. Grain size analyses of the coarsefraction suggests there are two populations of clasts:one containing large blocks 2-8 m in diameter andanother dominated by clasts <25 cm in diameter. Thediamictite bed also contains accretionary blocks, up to4.5 m in diameter. The base of the diamictite bed onlyrarely exhibits evidence of shear and appears to havebeen mostly emplaced by a turbulent flow over thespheroid bed. One location in Mexico exposes an ~100m long horizontal shear plane separating two flowswithin the diamictite bed.Conclusions: Comparisons of the Chicxulubcontinuous ejecta blanket with crater scalingrelationships clearly show that the thickness and extentof ejecta blankets from large lunar craters do notcompare well with Chicxulub. The Chicxulub ejectablanket extends farther and contains more materialLunar and Planetary Science XXX" @default.
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• W63144865 date "1999-03-01" @default.
• W63144865 modified "2023-09-25" @default.
• W63144865 title "The Chicxulub Continuous Ejecta Blanket and Its Implications for Fluidized Ejecta Blankets on Mars" @default.
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