Identification of mineral impactors in hypervelocity impact craters in aluminum by Raman spectroscopy of residues

Burchell, M. J.; Foster, N. J.; Kearsley, A. T.; Creighton, J. A.

doi:10.1111/j.1945-5100.2008.tb00614.x

Cited by 24 publications

(31 citation statements)

References 20 publications

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“…This is consistent with the previous reports of recovery of crystalline fragments of larger (>20 μm) mineral projectiles in impacts on aluminum at 6 km s −1 (see Burchell et al. ), wherein Raman spectroscopy confirmed that surviving crystalline material was present. In that article, Raman spectroscopy was conducted on the fragments indicating the presence of crystalline material in the residue, and their unmelted nature was implied by survival of rod shaped fragments of wollastonite whose orientation was aligned with the main axis of an elliptical crater, a result confirmed by TEM analyses (Wozniakiewicz et al.…”

Section: Discussionsupporting

confidence: 92%

Survival of refractory presolar grain analogs during Stardust‐like impact into Al foils: Implications for Wild 2 presolar grain abundances and study of the cometary fine fraction

Croat

Floss

Haas

et al. 2015

Meteorit & Planetary Scien

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We present results of FIB–TEM studies of 12 Stardust analog Al foil craters which were created by firing refractory Si and Ti carbide and nitride grains into Al foils at 6.05 km s−1 with a light‐gas gun to simulate capture of cometary grains by the Stardust mission. These foils were prepared primarily to understand the low presolar grain abundances (both SiC and silicates) measured by SIMS in Stardust Al foil samples. Our results demonstrate the intact survival of submicron SiC, TiC, TiN, and less‐refractory Si3N4 grains. In small (<2 μm) craters that are formed by single grain impacts, the entire impacting crystalline grain is often preserved intact with minimal modification. While they also survive in crystalline form, grains at the bottom of larger craters (>5 μm) are typically fragmented and are somewhat flattened in the direction of impact due to partial melting and/or plastic deformation. The low presolar grain abundance estimates derived from SIMS measurements of large craters (mostly >50 μm) likely result from greater modification of these impactors (i.e., melting and isotopic dilution), due to higher peak temperatures/pressures in these crater impacts. The better survivability of grains in smaller craters suggests that more accurate presolar grain estimates may be achievable through measurement of such craters. It also suggests small craters can provide a complementary method of study of the Wild 2 fine fraction, especially for refractory CAI‐like minerals.

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Section: Discussionsupporting

confidence: 92%

Survival of refractory presolar grain analogs during Stardust‐like impact into Al foils: Implications for Wild 2 presolar grain abundances and study of the cometary fine fraction

Croat

Floss

Haas

et al. 2015

Meteorit & Planetary Scien

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“…Thus, the use of non‐silica aerogel as a complementary capture medium to silica aerogel would expand the scientific value of any future particle capture of return missions. The fact that important results have been obtained from analyses of particles captured in the Stardust aluminum foil underscores the need for complementary capture media (Burchell et al. 2008; Kearsley et al.…”

Section: Introductionmentioning

confidence: 99%

Non-silica aerogels as hypervelocity particle capture materials

Jones¹

2010

Meteoritics and Planetary Science

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Abstract-The Stardust sample return mission to the comet Wild 2 used silica aerogel as the principal cometary and interstellar particle capture and return medium. However, since both cometary dust and interstellar grains are composed largely of silica, using a silica collector complicates the science that can be accomplished with these particles. The use of non-silica aerogel in future extra-terrestrial particle capture and return missions would expand the scientific value of these missions. Alumina, titania, germania, zirconia, tin oxide, and resorcinol ⁄ formaldehyde aerogels were produced and impact tested with 20, 50, and 100 lm glass microspheres to determine the suitability of different non-silica aerogels as hypervelocity particle capture mediums. It was found that non-silica aerogels do perform as efficient hypervelocity capture mediums, with alumina, zirconia, and resorcinol ⁄ formaldehyde aerogels proving to be the best of the materials tested.

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“…Another relevant observation is that of Burchell et al (2008b) where impacts into aluminium 1100 at 6.1 km s −1 not only yield residues from a variety of minerals but also Raman signals are obtained from projectile fragments in the craters. This was true for, amongst others, olivine and enstatite, although not for lizardite impactors.…”

Section: How Often Do Residues Remain?mentioning

confidence: 99%

In situ analysis of residues resulting from laboratory impacts into aluminum 1100 foil: Implications for Stardust crater analyses

Wozniakiewicz

Kearsley

Burchell

et al. 2009

Meteorit & Planetary Scien

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Abstract-The encounter between the Stardust spacecraft and particles from comet 81P/Wild 2 gave impacts at a relative velocity of 6.1 km s −1 and near perpendicular incidence to the collector surface. Such conditions are well within the performance limits of light gas gun laboratory simulations. For this study, two series of shots were conducted at the University of Kent, firing magnesium silicates (Mg end-member forsterite, enstatite, diopside and lizardite), followed by a suite of increasingly Ferich olivines (through to Fe end-member fayalite) into Stardust flight-spare foils. Preserved residues were analysed using scanning electron microscopy combined with energy dispersive X-ray analyses (SEM/EDX). X-ray count integrals show that mineral compositions remain distinct from one another after impact, although they do show increased scatter. However, there is a small but systematic increase in Mg relative to Si for all residues when compared to projectile compositions. While some changes in Mg:Si may be due to complex analytical geometries in craters, there appears to be some preferential loss of Si. In practice, EDX analyses in craters on Stardust Al 1100 foil inevitably include contributions from Fe-and Si-rich alloy inclusions, leading to further scattering of element ratios. Such inclusions have complicated Mg:Fe data interpretation. Compositional heterogeneity in the synthetic olivine projectiles also introduces data spread. Nevertheless, even with the preceding caveats, we find that the main groups of mafic silicates can be easily and reliably distinguished in EDX analyses performed in rapid surveys of foil craters, enabling access to a valuable additional collection of cometary materials.

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Identification of mineral impactors in hypervelocity impact craters in aluminum by Raman spectroscopy of residues

Cited by 24 publications

References 20 publications

Survival of refractory presolar grain analogs during Stardust‐like impact into Al foils: Implications for Wild 2 presolar grain abundances and study of the cometary fine fraction

Survival of refractory presolar grain analogs during Stardust‐like impact into Al foils: Implications for Wild 2 presolar grain abundances and study of the cometary fine fraction

Non-silica aerogels as hypervelocity particle capture materials

In situ analysis of residues resulting from laboratory impacts into aluminum 1100 foil: Implications for Stardust crater analyses

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