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Ultrafast growth of wadsleyite in shock-produced melts and its implications for early solar system impact processes

Tschauner, Oliver and Kostandova, Natalya and Ahrens, Thomas J. and Ma, Chi and Sinogeikin, Stanislas and Liu, Zhenxian and Fakra, Sirine and Tamura, Nobumichi and Asimow, Paul D. (2009) Ultrafast growth of wadsleyite in shock-produced melts and its implications for early solar system impact processes. Proceedings of the National Academy of Sciences of the United States of America, 106 (33). pp. 13691-13695. ISSN 0027-8424. PMCID PMC2728955. doi:10.1073/pnas.0905751106. https://resolver.caltech.edu/CaltechAUTHORS:20090908-083701874

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Abstract

We observed micrometer-sized grains of wadsleyite, a high-pressure phase of (Mg,Fe)_2SiO_4, in the recovery products of a shock experiment. We infer these grains crystallized from shock-generated melt over a time interval of <1 μs, the maximum time over which our experiment reached and sustained pressure sufficient to stabilize this phase. This rapid crystal growth rate (≈1 m/s) suggests that, contrary to the conclusions of previous studies of the occurrence of high-pressure phases in shock-melt veins in strongly shocked meteorites, the growth of high-pressure phases from the melt during shock events is not diffusion-controlled. Another process, such as microturbulent transport, must be active in the crystal growth process. This result implies that the times necessary to crystallize the high-pressure phases in shocked meteorites may correspond to shock pressure durations achieved on impacts between objects 1–5 m in diameter and not, as previously inferred, ≈1–5 km in diameter. These results may also provide another pathway for syntheses, via shock recovery, of some high-value, high-pressure phases.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1073/pnas.0905751106DOIArticle
http://www.pnas.org/content/106/33/13691.abstractPublisherArticle
http://www.ncbi.nlm.nih.gov/pmc/articles/PMC2728955/PubMed CentralArticle
ORCID:
AuthorORCID
Tschauner, Oliver0000-0003-3364-8906
Ma, Chi0000-0002-1828-7033
Tamura, Nobumichi0000-0002-3698-2611
Asimow, Paul D.0000-0001-6025-8925
Additional Information:Copyright ©2009 by the National Academy of Sciences. Contributed by Thomas J. Ahrens, June 17, 2009 (received for review June 20, 2008). Published online before print August 10, 2009, doi: 10.1073/pnas.0905751106 We thank M. Long, E. Gelle, R. Oliver, E. Miura, and G. Rossman for experimental and analytical support. This work was supported by National Science Foundation Grant 0552010, National Nuclear Security Administration Cooperative Agreement DOE-FC88-01NV14049, and National Aeronautics and Space Administration/Goddard Grants NNG04GP57G and NNG04GI07G. N.K. was supported by the California Institute of Technology Summer Undergraduate Research Fellowships program and Mr. and Mrs. Robert E. Anderson. The High Pressure Collaborative Access Team facility was supported by the Department of Energy-Basic Energy Sciences, Department of Energy-National Nuclear Security Administration, National Science Foundation, Department of Defense-Army Tank-Automotive and Armaments Command, and the W. M. Keck Foundation. The U2A beamline is supported by the Consortium for Materials Properties Research in Earth Sciences under National Science Foundation Cooperative Agreement 06-49658, Department of Energy Grant DE-FC52-08NA28554. Advanced Photon Source, Advanced Light Source, and National Synchrotron Light Source are supported by the Department of Energy-Basic Energy Sciences under Contracts W-31-109-Eng-38, DE-AC02–05CH11231, and DE AC02-98CH10886, respectively. Field emission scanning electron microscopy, EBSD, and EMP analyses were carried out at the California Institute of Technology Geological and Planetary Sciences Division Analytical Facility, which is supported in part by National Science Foundation Grant EAR-0318518 and the National Science Foundation Materials Research Science and Engineering Center Program under Grant DMR-00800065. Author contributions: O.T., P.D.A., and T.J.A. designed research; O.T., P.D.A., N.K., C.M., S.S., Z.L., S.F., and N.T. performed research; O.T., P.D.A., and N.K. contributed new reagents/analytic tools; O.T., P.D.A., and N.K. analyzed data; and O.T., P.D.A., N.K., and T.J.A. wrote the paper. The authors declare no conflict of interest.
Funders:
Funding AgencyGrant Number
NSF0552010
National Nuclear Security AdministrationDOE-FC88-01NV14049
NASANNG04GP57G
NASANNG04GI07G
Caltech Summer Undergraduate Research Fellowship (SURF)UNSPECIFIED
Mr. and Mrs. Robert E. AndersonUNSPECIFIED
Department of Energy (DOE)DE-FC52-08NA28554
Department of DefenseUNSPECIFIED
W. M. Keck FoundationUNSPECIFIED
NSF06-49658
Department of Energy (DOE)W-31-109-ENG-38
Department of Energy (DOE)DE-AC02–05CH11231
Department of Energy (DOE)DE-AC02-98CH10886
NSFEAR-0318518
NSFDMR-00800065
Subject Keywords:meteorite; recovery; high-pressure phases; planetesimal growth; shock experiments
Issue or Number:33
PubMed Central ID:PMC2728955
DOI:10.1073/pnas.0905751106
Record Number:CaltechAUTHORS:20090908-083701874
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20090908-083701874
Official Citation:Oliver Tschauner, Paul D. Asimow, Natalya Kostandova, Thomas J. Ahrens, Chi Ma, Stanislas Sinogeikin, Zhenxian Liu, Sirine Fakra, and Nobumichi Tamura Ultrafast growth of wadsleyite in shock-produced melts and its implications for early solar system impact processes PNAS 2009 106 (33) 13691-13695; published ahead of print August 10, 2009, doi:10.1073/pnas.0905751106
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:15640
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:08 Sep 2009 19:34
Last Modified:08 Nov 2021 23:21

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