Please use this identifier to cite or link to this item: http://hdl.handle.net/1893/27356
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dc.contributor.authorTait, Alastair Wen_UK
dc.contributor.authorFisher, Kent Ren_UK
dc.contributor.authorSrinivasan, Poornaen_UK
dc.contributor.authorSimon, Justin Ien_UK
dc.date.accessioned2018-06-12T00:00:11Z-
dc.date.available2018-06-12T00:00:11Z-
dc.date.issued2016-11-15en_UK
dc.identifier.urihttp://hdl.handle.net/1893/27356-
dc.description.abstractCarbonaceous chondrites, such as those associated with the Vigarano (CV) parent body, exhibit a diverse range of oxidative/reduced alteration mineralogy (McSween, 1977). Although fluids are often cited as the medium by which this occurs (Rubin, 2012), a mechanism to explain how this fluid migrates, and why some meteorite subtypes from the same planetary body are more oxidized than others remains elusive. In our study we examined a slab of the well-known Allende (CV3OxA) meteorite. Using several petrological techniques (e.g., Fry's and Flinn) and Computerized Tomography (CT) we discover it exhibits a strong penetrative planar fabric, resulting from strain partitioning among its major components: Calcium–Aluminum-rich Inclusions (CAIs) (64.5%CT) > matrix (21.5%Fry) > chondrules (17.6%CT). In addition to the planar fabric, we found a strong lineation defined by the alignment of the maximum elongation of flattened particles interpreted to have developed by an impact event. The existence of a lineation could either be non-coaxial deformation, or the result of a mechanically heterogeneous target material. In the later case it could have formed due to discontinuous patches of sub-surface ice and/or fabrics developed through prior impact compaction (MacPherson and Krot, 2014), which would have encouraged preferential flow within the target material immediately following the impact, compacting pore spaces. We suggest that structurally controlled movement of alteration fluids in the asteroid parent body along pressure gradients contributed to the formation of secondary minerals, which may have ultimately lead to the different oxidized subtypes.en_UK
dc.language.isoenen_UK
dc.publisherElsevier BVen_UK
dc.relationTait AW, Fisher KR, Srinivasan P & Simon JI (2016) Evidence for impact induced pressure gradients on the Allende CV3 parent body: Consequences for fluid and volatile transport. Earth and Planetary Science Letters, 454, pp. 213-224. https://doi.org/10.1016/j.epsl.2016.09.015en_UK
dc.rightsPublished by Elsevier B.V. This is an open access article under the CC BY-NC-ND license (http://creativecommons.org/licenses/by-nc-nd/4.0/).en_UK
dc.rights.urihttp://creativecommons.org/licenses/by-nc-nd/4.0/en_UK
dc.subjectmeteoriteen_UK
dc.subjectpetrofabricen_UK
dc.subjectlineationen_UK
dc.subjectfoliationen_UK
dc.subjectdeformationen_UK
dc.subjectfluiden_UK
dc.titleEvidence for impact induced pressure gradients on the Allende CV3 parent body: Consequences for fluid and volatile transporten_UK
dc.typeJournal Articleen_UK
dc.identifier.doi10.1016/j.epsl.2016.09.015en_UK
dc.citation.jtitleEarth and Planetary Science Lettersen_UK
dc.citation.issn0012-821Xen_UK
dc.citation.volume454en_UK
dc.citation.spage213en_UK
dc.citation.epage224en_UK
dc.citation.publicationstatusPublisheden_UK
dc.citation.peerreviewedRefereeden_UK
dc.type.statusVoR - Version of Recorden_UK
dc.contributor.funderNational Aeronautics and Space Administrationen_UK
dc.citation.date30/06/2016en_UK
dc.contributor.affiliationMonash Universityen_UK
dc.contributor.affiliationUniversity of Cincinnatien_UK
dc.contributor.affiliationUniversity of New Mexico, USAen_UK
dc.contributor.affiliationNASA Johnson Space Centeren_UK
dc.identifier.isiWOS:000386645700022en_UK
dc.identifier.scopusid2-s2.0-84992188016en_UK
dc.identifier.wtid920654en_UK
dc.contributor.orcid0000-0001-7571-3169en_UK
dc.date.accepted2016-09-08en_UK
dc.date.filedepositdate2018-06-11en_UK
Appears in Collections:Biological and Environmental Sciences Journal Articles

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