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Final reports of the Stardust Interstellar Preliminary Examination

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Hoppe,  Peter
Particle Chemistry, Max Planck Institute for Chemistry, Max Planck Society;

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Huth,  Joachim
Particle Chemistry, Max Planck Institute for Chemistry, Max Planck Society;

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Leitner,  Jan
Particle Chemistry, Max Planck Institute for Chemistry, Max Planck Society;

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Westphal, A. J., Bechtel, H. A., Brenker, F. E., Butterworth, A. L., Flynn, G., Frank, D. R., et al. (2014). Final reports of the Stardust Interstellar Preliminary Examination. Meteoritics & Planetary Science, 49(9), 1720-1733. doi:10.1111/maps.12221.


Cite as: http://hdl.handle.net/11858/00-001M-0000-0024-B695-1
Abstract
With the discovery of bona fide extraterrestrial materials in the Stardust Interstellar Dust Collector, NASA now has a fundamentally new returned sample collection, after the Apollo, Antarctic meteorite, Cosmic Dust, Genesis, Stardust Cometary, Hayabusa, and Exposed Space Hardware samples. Here, and in companion papers in this volume, we present the results from the Preliminary Examination of this collection, the Stardust Interstellar Preliminary Examination (ISPE). We found extraterrestrial materials in two tracks in aerogel whose trajectories and morphology are consistent with an origin in the interstellar dust stream, and in residues in four impacts in the aluminum foil collectors. While the preponderance of evidence, described in detail in companion papers in this volume, points toward an interstellar origin for some of these particles, alternative origins have not yet been eliminated, and definitive tests through isotopic analyses were not allowed under the terms of the ISPE. In this summary, we answer the central questions of the ISPE: How many tracks in the collector are consistent in their morphology and trajectory with interstellar particles? How many of these potential tracks are consistent with real interstellar particles, based on chemical analysis? Conversely, what fraction of candidates are consistent with either a secondary or interplanetary origin? What is the mass distribution of these particles, and what is their state? Are they particulate or diffuse? Is there any crystalline material? How many detectable impact craters (> 100 nm) are there in the foils, and what is their size distribution? How many of these craters have analyzable residue that is consistent with extraterrestrial material? And finally, can craters from secondaries be recognized through crater morphology (e.g., ellipticity)?