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dc.contributor.advisorLewis, John S.en_US
dc.contributor.authorHutson, Melinda Lee, 1953-
dc.creatorHutson, Melinda Lee, 1953-en_US
dc.date.accessioned2013-05-09T11:33:21Z
dc.date.available2013-05-09T11:33:21Z
dc.date.issued1996en_US
dc.identifier.urihttp://hdl.handle.net/10150/290633
dc.description.abstractThe unique mineral and chemical composition of enstatite chondrites has been difficult to explain. Contrary to the conclusions of other workers, there is no evidence for a significant chemical difference between EH and EL chondrites, except in bulk S. Analyzed splits of the enstatite chondrites vary widely in major element composition, largely as a result of analyzing inadequate sample sizes. The phases in enstatite chondrites most likely to reflect conditions in the solar nebula include enstatite, forsterite, diopside, silica polymorph, albite, metal, troilite, oldhamite, niningerite, schreibersite, minerals A and B, caswellsilverite, and djerfisherite. There is evidence that the enstatite chondrites did not form in complete equilibrium. The Na-Cr sulfides known as minerals A and B contain oxygen, but contain little hydrogen, indicating that these sulfides did not necessarily form under hydrous conditions. The mineralogy and modal composition of type 3 enstatite chondrites are best matched by thermodynamic models that involve two chemical fractionations from a gas of solar or cosmic composition. The first fractionation entailed the removal from the enstatite chondrite formation location of solids in equilibrium with a solar composition gas at ∼1270K. The second fractionation involved the subsequent removal of water vapor from the enstatite chondrite formation location. These fractionations can be understood if the enstatite chondrites formed in a water-depleted gas from which solids at 1270K had been previously removed, sunward of a water condensation front in the solar nebula. Enstatite chondrites largely equilibrated in the nebula at ∼925K, although sulfidation of metal occurred to temperatures as low as ∼675K.
dc.language.isoen_USen_US
dc.publisherThe University of Arizona.en_US
dc.rightsCopyright © is held by the author. Digital access to this material is made possible by the University Libraries, University of Arizona. Further transmission, reproduction or presentation (such as public display or performance) of protected items is prohibited except with permission of the author.en_US
dc.subjectGeology.en_US
dc.subjectGeochemistry.en_US
dc.titleChemical studies of enstatite chondritesen_US
dc.typetexten_US
dc.typeDissertation-Reproduction (electronic)en_US
thesis.degree.grantorUniversity of Arizonaen_US
thesis.degree.leveldoctoralen_US
dc.identifier.proquest9713420en_US
thesis.degree.disciplineGraduate Collegeen_US
thesis.degree.disciplinePlanetary Sciencesen_US
thesis.degree.namePh.D.en_US
dc.identifier.bibrecord.b34417424en_US
refterms.dateFOA2018-08-29T20:54:52Z
html.description.abstractThe unique mineral and chemical composition of enstatite chondrites has been difficult to explain. Contrary to the conclusions of other workers, there is no evidence for a significant chemical difference between EH and EL chondrites, except in bulk S. Analyzed splits of the enstatite chondrites vary widely in major element composition, largely as a result of analyzing inadequate sample sizes. The phases in enstatite chondrites most likely to reflect conditions in the solar nebula include enstatite, forsterite, diopside, silica polymorph, albite, metal, troilite, oldhamite, niningerite, schreibersite, minerals A and B, caswellsilverite, and djerfisherite. There is evidence that the enstatite chondrites did not form in complete equilibrium. The Na-Cr sulfides known as minerals A and B contain oxygen, but contain little hydrogen, indicating that these sulfides did not necessarily form under hydrous conditions. The mineralogy and modal composition of type 3 enstatite chondrites are best matched by thermodynamic models that involve two chemical fractionations from a gas of solar or cosmic composition. The first fractionation entailed the removal from the enstatite chondrite formation location of solids in equilibrium with a solar composition gas at ∼1270K. The second fractionation involved the subsequent removal of water vapor from the enstatite chondrite formation location. These fractionations can be understood if the enstatite chondrites formed in a water-depleted gas from which solids at 1270K had been previously removed, sunward of a water condensation front in the solar nebula. Enstatite chondrites largely equilibrated in the nebula at ∼925K, although sulfidation of metal occurred to temperatures as low as ∼675K.


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