Impact melting of carbonates from the Chicxulub crater

Jones, Adrian P.; Claeys, Philippe; Heuschkel, S.

doi:10.1007/bfb0027767

Cited by 34 publications

(67 citation statements)

References 28 publications

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“…CL in calcite has been described as characteristically orange to yellow, while dolomite tends to show red CL (Adams and MacKenzie 1998). Shock-melted carbonates have been reported to show a strong luminescence-quenching effect due to the mixing of iron into carbonate melt (Jones et al 2000). Schulte (2003) ascribed dull red-brown CL and a lack of CL to quenched carbonate melts associated with impactgenerated spherules.…”

Section: Samples and Methodsmentioning

confidence: 99%

Impact‐related dike breccia lithologies in the ICDP drill core Yaxcopoil‐1, Chicxulub impact structure, Mexico

Wittmann

Kenkmann

Schmitt

et al. 2004

Meteorit & Planetary Scien

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Abstract-Petrographic descriptions of three dike breccia lithologies from drill core Yaxcopoil-1 (Yax-1) are presented. They occur within allochthonous units of displaced sedimentary megablocks of the Chicxulub impact structure. The suevitic dike breccias are the uppermost dike lithology. They contain melt rock particles and melt injections into the dike groundmass. Shock features occur ubiquitously and indicate a strong thermal annealing. Flow textures suggest a highly energetic emplacement process, possibly during the excavation stage as a ground-surge related deposit. The impact melt rock dikes are present in a strongly brecciated megablock interval as flow textured, anastomozing veinlets of impact melt rock that were altered to clay minerals. The melt impregnated a dolomitic host rock, indicating a low viscosity and, thus, high initial temperatures. Brecciation of the impact melt rock dikes occurred while they were still below the glass transition temperature, suggesting that dynamic conditions prevailed shortly after the emplacement process. Major element data indicates that the impact melt rock dikes differ in composition from the homogenized impact melt rock of Chicxulub. This could point to an emplacement during the late compression or early excavation stages of cratering. The clastic polymict dike breccias are coeval with pervasive brittle fracturing of the host rocks. They bear clasts including some crystalline basement and possible melt rock particles in a fine-grained dolomite matrix with turbulent flow textures. Fabric and texture indicate a granular flow at ambient pressures. Such conditions could be envisaged for the excavation phase while the transient cavity grew and fractures opened.

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Section: Samples and Methodsmentioning

confidence: 99%

Impact‐related dike breccia lithologies in the ICDP drill core Yaxcopoil‐1, Chicxulub impact structure, Mexico

Wittmann

Kenkmann

Schmitt

et al. 2004

Meteorit & Planetary Scien

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“…The calcite and silicate glass of the groundmass of these impactites represent a series of impact-generated melts that were molten at the time of, and after, deposition. In any model that involves some component of ballistic ejection and transport through the atmosphere, silicate melt would be quenched to a glass before deposition and carbonate melt would have crystallized (e.g., the feathery-textured carbonates in ejecta at the Chicxulub impact structure, Mexico; Jones et al 2000). 3.…”

Section: Impact Melt Breccias Of the Near-surface Crater Rim Regionmentioning

confidence: 99%

“…These impactites can, therefore, be termed impact melt breccias or clast-rich impact melt rocks (Osinski andSpray 2001, 2003), according to the terminology of Grieve (1994, 1996). Carbonate melt-rich impactites have also been documented at the Ries (Graup 1999;Osinski 2003;Osinski et al 2004) and Chicxulub (Jones et al 2000;Claeys et al 2003;Dressler et al 2004;Kring et al 2004;Stˆffler et al 2004;Tuchscherer et al 2004) impact structures.…”

Section: Introductionmentioning

confidence: 99%

Impactites of the Haughton impact structure, Devon Island, Canadian High Arctic

Osinski

Spray

Lee

2005

Meteoritics &Amp; Planetary Science

123

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Abstract-Contrary to the previous interpretation of a single allochthonous impactite lithology, combined field, optical, and analytical scanning electron microscopy (SEM) studies have revealed the presence of a series of impactites at the Haughton impact structure. In the crater interior, there is a consistent upward sequence from parautochthonous target rocks overlain by parautochthonous lithic (monomict) breccias, through allochthonous lithic (polymict) breccia, into pale grey allochthonous impact melt breccias. The groundmass of the pale grey impact melt breccias consists of microcrystalline calcite, silicate impact melt glass, and anhydrite. Analytical data and microtextures indicate that these phases represent a series of impact-generated melts that were molten at the time of, and following, deposition. Impact melt glass clasts are present in approximately half of the samples studied. Consideration of the groundmass phases and impact glass clasts reveal that impactites of the crater interior contain shock-melted sedimentary material from depths of >920 to <1880 m in the preimpact target sequence. Two principal impactites have been recognized in the near-surface crater rim region of Haughton. Pale yellow-brown allochthonous impact melt breccias and megablocks are overlain by pale grey allochthonous impact melt breccias. The former are derived from depths of >200 to <760 m and are interpreted as remnants of the continuous ejecta blanket. The pale grey impact melt breccias, although similar to the impact melt breccias of the crater interior, are more carbonate-rich and do not appear to have incorporated clasts from the crystalline basement. Thus, the spatial distribution of the crater-fill impactites at Haughton, the stratigraphic succession from target rocks to allochthonous impactites, the recognition of large volumes of impact melt breccias, and their probable original volume are all analogous to characteristics of coherent impact melt layers in comparatively sized structures formed in crystalline targets.

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“…Nevertheless, the small calcium carbonate particles in aerogel still gave recognizable carbonate Raman spectra. Separately, we note that recent experimental evidence strongly suggests that, for example, carbonate minerals (such as calcite) do not undergo substantial dissociation and loss of carbon dioxide even at the peak shock pressures experienced during hypervelocity impact (Jones et al 2000).…”

Section: Mineral Categorizationmentioning

confidence: 69%

Identification of minerals and meteoritic materials via Raman techniques after capture in hypervelocity impacts on aerogel

Burchell

Mann

Creighton

et al. 2006

Meteorit & Planetary Scien

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Abstract-Mineral particles analogous to components of cosmic dust were tested to determine if their Raman signatures can be recognized after hypervelocity capture in aerogel. The mineral particles were accelerated onto the silica aerogel by light-gas-gun shots. It was found that all the individual minerals captured in aerogel could be identified using Raman (or fluorescence) spectra. The laser beam spot size was ∼5 micrometers, and in some cases the captured particles were of a similar small size. In some samples fired into aerogel, a broadening and a shift in the wave numbers of some of the Raman bands was observed, a result of the trapped particles being at elevated temperatures due to laser heating. Temperatures of samples were also estimated from the relative intensities of Stokes and anti-Stokes Raman bands, or, in the case of corundum particles, from the wave number of fluorescence bands excited by the laser. The temperature varied greatly, dependent upon laser power and the nature of the particle. Most of the mineral particles examined had temperatures below 200 °C at a laser power of about 3 mW at the sample. This temperature is sufficiently low enough not to damage most materials expected to be found captured in aerogel in space. In the worst case, some particles were shown to have temperatures of 500-700 °C. In addition, selected meteorite samples were examined to obtain Raman signatures of their constituent minerals and were then shot into aerogel. It was possible to find Raman signatures after capture in aerogel and obtain a Raman map of a whole grain in situ in the aerogel. It is concluded that Raman analysis is indeed well suited for an in situ analysis of micrometer-sized materials captured in aerogel.

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Impact melting of carbonates from the Chicxulub crater

Cited by 34 publications

References 28 publications

Impact‐related dike breccia lithologies in the ICDP drill core Yaxcopoil‐1, Chicxulub impact structure, Mexico

Impact‐related dike breccia lithologies in the ICDP drill core Yaxcopoil‐1, Chicxulub impact structure, Mexico

Impactites of the Haughton impact structure, Devon Island, Canadian High Arctic

Identification of minerals and meteoritic materials via Raman techniques after capture in hypervelocity impacts on aerogel

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