McKeegan, Kevin D. and Aléon, Jerome and Bradley, John and Brownlee, Donald and Busemann, Henner and Butterworth, Anna and Chaussidon, Marc and Fallon, Stewart and Floss, Christine and Gilmour, Jamie and Gounelle, Matthieu and Graham, Giles and Guan, Yunbin and Heck, Philipp R. and Hoppe, Peter and Hutcheon, Ian D. and Huth, Joachim and Ishii, Hope and Ito, Motoo and Jacobsen, Stein B. and Kearsley, Anton and Leshin, Laurie A. and Liu, Ming-Chang and Lyon, Ian and Marhas, Kuljeet and Marty, Bernard and Matrajt, Graciela and Meibom, Anders and Messenger, Scott and Mostefaoui, Smail and Mukhopadhyay, Sujoy and Nakamura-Messenger, Keiko and NIttler, Larry and Palma, Russ and Pepin, Robert O. and Papanastassiou, Dimitri A. and Robert, François and Schlutter, Dennis and Snead, Christopher J. and Stadermann, Frank J. and Stroud, Rhonda and Tsou, Peter and Westphal, Andrew and Young, Edward D. and Ziegler, Karen and Zimmerman, Laurent and Zinner, Ernst (2006) Isotopic Compositions of Cometary Matter Returned by Stardust. Science, 314 (5806). pp. 1724-1728. ISSN 0036-8075. doi:10.1126/science.1135992. https://resolver.caltech.edu/CaltechAUTHORS:20141118-081613400
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Abstract
Hydrogen, carbon, nitrogen, and oxygen isotopic compositions are heterogeneous among comet 81P/Wild 2 particle fragments; however, extreme isotopic anomalies are rare, indicating that the comet is not a pristine aggregate of presolar materials. Nonterrestrial nitrogen and neon isotope ratios suggest that indigenous organic matter and highly volatile materials were successfully collected. Except for a single ^(17)O-enriched circumstellar stardust grain, silicate and oxide minerals have oxygen isotopic compositions consistent with solar system origin. One refractory grain is ^(16)O-enriched, like refractory inclusions in meteorites, suggesting that Wild 2 contains material formed at high temperature in the inner solar system and transported to the Kuiper belt before comet accretion.
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| Additional Information: | © 2006 American Association for the Advancement of Science. Received 6 October 2006; accepted 17 November 2006. We thank D. Burnett and G. J. Wasserburg for helpful advice and encouragement during the Preliminary Examination. We acknowledge financial support from the NASA Cosmochemistry Program, the NASA Sample Return Laboratory Instrumentation and Data Analysis Program, the Stardust Participating Scientist Program, the NSF Instrumentation and Facilities Program, the Particle Physics and Astronomy Research Council, the Centre National d'Etudes Spatiales, the CNRS France Etats-Unis program, and the Région Lorraine. Aspects of this work were performed under the auspices of the U.S. Department of Energy by the University of California, Lawrence Livermore National Laboratory, under Contract No. W-7405-Eng-48. We also thank the scientists and engineers at the Jet Propulsion Laboratory and at Lockheed Martin Astronautics whose dedication and skill brought these precious samples back to Earth. | ||||||||||||||||||||||||||||||||||||||||||||||||||||||
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| Issue or Number: | 5806 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||
| DOI: | 10.1126/science.1135992 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Record Number: | CaltechAUTHORS:20141118-081613400 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Persistent URL: | https://resolver.caltech.edu/CaltechAUTHORS:20141118-081613400 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Usage Policy: | No commercial reproduction, distribution, display or performance rights in this work are provided. | ||||||||||||||||||||||||||||||||||||||||||||||||||||||
| ID Code: | 51880 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Collection: | CaltechAUTHORS | ||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited By: | Tony Diaz | ||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Deposited On: | 18 Nov 2014 17:00 | ||||||||||||||||||||||||||||||||||||||||||||||||||||||
| Last Modified: | 08 Mar 2023 20:25 |
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