Stardust Interstellar Preliminary Examination V: XRF analyses of interstellar dust candidates at ESRF ID13

Brenker, Frank E. and Westphal, Andrew J. and Vincze, Laszlo and Burghammer, Manfred and Schmitz, Sylvia and Schoonjans, Tom and Silversmit, Geert and Vekemans, Bart and Allen, Carlton and Anderson, David and Ansari, Asna and Bajt, Saša and Bastien, Ron K. and Bassim, Nabil and Bechtel, Hans A. and Borg, Janet and Bridges, John and Brownlee, Donald E. and Burchell, Mark J. and Butterworth, Anna L. and Changela, Hitesh and Cloetens, Peter and Davis, Andrew M. and Doll, Ryan and Floss, Christine and Flynn, George and Fougeray, Patrick and Frank, David R. and Gainsforth, Zack and Grün, Eberhard and Heck, Philipp R. and Hillier, Jon K. and Hoppe, Peter and Hudson, Bruce and Huth, Joachim and Hvide, Brit and Kearsley, Anton and King, Ashley J. and Lai, Barry and Leitner, Jan and Lemelle, Laurence and Leroux, Hugues and Leonard, Ariel and Lettieri, Robert and Marchant, William and Nittler, Larry R. and Ogliore, Ryan and Ong, Wei Ja and Postberg, Frank and Price, Mark C. and Sandford, Scott A. and Tresseras, Juan-Angel Sans and Simionovici, Alexandre S. and Solé, Vicente A. and Srama, Ralf and Stadermann, Frank and Stephan, Thomas and Sterken, Veerle J. and Stodolna, Julien and Stroud, Rhonda M. and Sutton, Steven and Trieloff, Mario and Tsou, Peter and Tsuchiyama, Akira and Tyliszczak, Tolek and Von Korff, Joshua and Wordsworth, Naomi and Zevin, Daniel and Zolensky, Michael E. (2014) Stardust Interstellar Preliminary Examination V: XRF analyses of interstellar dust candidates at ESRF ID13. Meteoritics and Planetary Science, 49 (9). pp. 1594-1611. ISSN 1086-9379. (doi:https://doi.org/10.1111/maps.12206) (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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http://doi.org/10.1111/maps.12206

Abstract

Here, we report analyses by synchrotron X-ray fluorescence microscopy of the elemental composition of eight candidate impact features extracted from the Stardust Interstellar Dust Collector (SIDC). Six of the features were unambiguous tracks, and two were crater-like features. Five of the tracks are so-called “midnight” tracks—that is, they had trajectories consistent with an origin either in the interstellar dust stream or as secondaries from impacts on the Sample Return Capsule (SRC). In a companion paper reporting synchrotron X-ray diffraction analyses of ISPE candidates, we show that two of these particles contain natural crystalline materials: the terminal particle of track 30 contains olivine and spinel, and the terminal particle of track 34 contains olivine. Here, we show that the terminal particle of track 30, Orion, shows elemental abundances, normalized to Fe, that are close to CI values, and a complex, fine-grained structure. The terminal particle of track 34, Hylabrook, shows abundances that deviate strongly from CI, but shows little fine structure and is nearly homogenous. The terminal particles of other midnight tracks, 29 and 37, had heavy element abundances below detection threshold. A third, track 28, showed a composition inconsistent with an extraterrestrial origin, but also inconsistent with known spacecraft materials. A sixth track, with a trajectory consistent with secondary ejecta from an impact on one of the spacecraft solar panels, contains abundant Ce and Zn. This is consistent with the known composition of the glass covering the solar panel. Neither crater-like feature is likely to be associated with extraterrestrial materials. We also analyzed blank aerogel samples to characterize background and variability between aerogel tiles. We found significant differences in contamination levels and compositions, emphasizing the need for local background subtraction for accurate quantification.

Item Type: Article
Divisions: Faculties > Sciences > School of Physical Sciences
Depositing User: Mark Burchell
Date Deposited: 23 Jan 2017 09:15 UTC
Last Modified: 25 Aug 2017 09:00 UTC
Resource URI: https://kar.kent.ac.uk/id/eprint/59994 (The current URI for this page, for reference purposes)
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