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

Wozniakiewicz, Penelope J., Kearsley, A.T., Burchell, Mark J., Foster, N.J., Cole, Mike J., Bland, P.A., Russell, S.S. (2009) In situ analysis of residues resulting from laboratory impacts into aluminum 1100 foil: Implications for Stardust crater analyses. Meteoritics and Planetary Science, 44 (10). pp. 1541-1559. ISSN 1086-9379. E-ISSN 1945-5100. (doi:10.1111/j.1945-5100.2009.tb01191.x) (The full text of this publication is not currently available from this repository. You may be able to access a copy if URLs are provided)

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Official URL
http://dx.doi.org/10.1111/j.1945-5100.2009.tb01191...

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 ay 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 AI 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 © The Meteoritical Society, 2009. Printed in USA.

Item Type: Article
DOI/Identification number: 10.1111/j.1945-5100.2009.tb01191.x
Additional information: Unmapped bibliographic data: LA - English [Field not mapped to EPrints] J2 - Meteorit. Planet. Sci. [Field not mapped to EPrints] AD - Impacts and Astromaterials Research Centre (IARC), Department of Mineralogy, Natural History Museum (NHM), London SW7 5BD, United Kingdom [Field not mapped to EPrints] AD - IARC, Imperial College London, South Kensington Campus, London SW11 2AZ, United Kingdom [Field not mapped to EPrints] AD - Centre for Astrophysics and Planetary Science, School of Physical Sciences, University of Kent, Canterbury, Kent CT2 7NH, United Kingdom [Field not mapped to EPrints] DB - Scopus [Field not mapped to EPrints] M3 - Article [Field not mapped to EPrints]
Subjects: Q Science > QB Astronomy > QB651 Planets, Minor
Divisions: Faculties > Sciences > School of Physical Sciences > Centre for Astrophysics and Planetary Sciences
Depositing User: Giles Tarver
Date Deposited: 29 Jan 2016 10:32 UTC
Last Modified: 01 Aug 2019 10:40 UTC
Resource URI: https://kar.kent.ac.uk/id/eprint/53884 (The current URI for this page, for reference purposes)
Burchell, Mark J.: https://orcid.org/0000-0002-2680-8943
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