Dust Production from the Hypervelocity Impact Disruption of Hydrated Targets

Flynn, G. J.; Durda, D. D.; Sandel, L. E.; Strait, M. M.

doi:10.1007/s11038-006-9100-z

Cited by 7 publications

(3 citation statements)

References 9 publications

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“…This suggests that intergranular fracture dominates at grain sizes <100 μm while transgranular fracture dominates at coarser scales (>100 μm). The grain size of the Winchcombe cataclastic matrix therefore closely agrees with the debris distributions generated by hypervelocity impact experiments into CM chondrites (Flynn et al., 2005, 2009; Tomeoka et al., 2003).…”

Section: Discussionsupporting

confidence: 79%

“…Impact experiments (~5 km s −1 ) into wet sandstone targets demonstrate that pore water reduces the peak pressure experienced at grain boundaries, thereby inhibiting grain comminution (transgranular fracture) while reducing shock wave attenuation, allowing for deeper penetration into the target (Baldwin et al, 2007;Buhl et al, 2013). Experimental studies impacting hydrated CM chondrites have concluded that these meteorites preferentially respond by catastrophic disruption even at relatively low velocities (2 km s −1 ; Flynn et al, 2009), producing abundant small fragments (<100 μm; Flynn et al, 2005Flynn et al, , 2009Tomeoka et al, 2003). Tomeoka et al (2003) explored higher peak pressures and demonstrated that phyllosilicate minerals experience thermal decomposition above 30 GPa.…”

Section: The Cataclastic Matrix and Parent Body Brecciationmentioning

confidence: 99%

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The Winchcombe meteorite—A regolith breccia from a rubble pile CM chondrite asteroid

Suttle

Daly

Jones

et al. 2022

Meteorit & Planetary Scien

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The Winchcombe meteorite is a CM chondrite breccia composed of eight distinct lithological units plus a cataclastic matrix. The degree of aqueous alteration varies between intensely altered CM2.0 and moderately altered CM2.6. Although no lithology dominates, three heavily altered rock types (CM2.1-2.3) represent >70 area%. Tochilinite-cronstedtite intergrowths (TCIs) are common in several lithologies. Their compositions can vary significantly, even within a single lithology, which can prevent a clear assessment of alteration extent if only TCI composition is considered. We suggest that this is due to early alteration under localized geochemical microenvironments creating a diversity of compositions and because later reprocessing was incomplete, leaving a record of the parent body's fluid history. In Winchcombe, the fragments of primary accretionary rock are held within a cataclastic matrix (~15 area%). This material is impact-derived fallback debris. Its grain size and texture suggest that the disruption of the original parent asteroid responded by intergranular fracture at grain sizes <100 μm, while larger phases, such as whole chondrules, splintered apart. Reaccretion formed a poorly lithified body. During atmospheric entry, the Winchcombe meteoroid broke apart with new fractures preferentially cutting through the weaker cataclastic

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Section: Discussionsupporting

confidence: 79%

Section: The Cataclastic Matrix and Parent Body Brecciationmentioning

confidence: 99%

The Winchcombe meteorite—A regolith breccia from a rubble pile CM chondrite asteroid

Suttle

Daly

Jones

et al. 2022

Meteorit & Planetary Scien

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show abstract

“…This emission is inhibited at dust grain sizes below the wavelength of the emission, so the technique is much less sensitive to sub-micron grains, and for larger grains the emission is proportional to the surface area of the grain, so surface area weighted abundances were reported rather than mass weighted abundances. Conversion to mass or molar fractions requires the assumption that all minerals have the same size-frequency distribution, but hypervelocity disruption experiments on different types of meteorites show different size-frequency distributions, suggesting the distribution may be different for different minerals (Flynn et al 2005). In addition, the best fit to the spectral data depends on the basis set of minerals selected for inclusion in the fitting routine.…”

Section: Mineralogymentioning

confidence: 99%

Cometary Dust

et al. 2018

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This review presents our understanding of cometary dust at the end of 2017. For decades, insight about the dust ejected by nuclei of comets had stemmed from remote observations from Earth or Earth's orbit, and from flybys, including the samples of dust returned to Earth for laboratory studies by the Stardust return capsule. The long-duration Rosetta mission has recently provided a huge and unique amount of data, obtained using numerous instruments, including innovative dust instruments, over a wide range of distances from the

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New estimates of the production of volatile gases from ablating carbonaceous micrometeoroids at Earth and Mars during an E-belt-type Late Heavy Bombardment

Court¹,

Sephton²

2014

Geochimica et Cosmochimica Acta

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Dust Production from the Hypervelocity Impact Disruption of Hydrated Targets

Cited by 7 publications

References 9 publications

The Winchcombe meteorite—A regolith breccia from a rubble pile CM chondrite asteroid

The Winchcombe meteorite—A regolith breccia from a rubble pile CM chondrite asteroid

Cometary Dust

New estimates of the production of volatile gases from ablating carbonaceous micrometeoroids at Earth and Mars during an E-belt-type Late Heavy Bombardment

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