Wade, J.; Hammond, S. J.; Rogers, N. W. and Grady, M. M.
|Google Scholar:||Look up in Google Scholar|
The enstatite chondrites are a group of metal- and sulphide-rich meteorites with a highly reduced composition. They have an oxygen isotope composition that is indistinguishable from that of the Earth-Moon system , and partly on this basis have been cited as model precursors for the Earth . However, it has proven difficult to reconcile the bulk elemental abundances of enstatite chondrites with those of the Earth. In order to explore any compositional link that enstatite meteorites may have with other planetary bodies, a good understanding of the range of their compositions is required. Previous work has used a variety of methods to determine the minor and trace element composition of these materials, with individual work often focusing upon either a restricted range of elements and/or a restricted number of meteorite samples. The highly reduced nature of the meteorites and the chemical reactivity of some of the meteorite components implies that only samples from falls should be considered for analysis. This, inevitably, makes drawing any conclusions from their bulk compositions somewhat difficult. Here we present compositional data from a comprehensive range of EH and EL meteorite falls, using a quadrupole ICPMS technique for trace element analysis, together with ICP–OES for the major elements. The aim is to provide an internally consistent data set for a large elemental range, such that better constraints may be placed both upon the models of enstatite chondrite formation, and their genetic relationship with other planetary bodies.
|Item Type:||Conference Item|
|Academic Unit/Department:||Faculty of Science, Technology, Engineering and Mathematics (STEM) > Physical Sciences
Faculty of Science, Technology, Engineering and Mathematics (STEM)
|Interdisciplinary Research Centre:||Centre for Earth, Planetary, Space and Astronomical Research (CEPSAR)|
|Depositing User:||Karen Guyler|
|Date Deposited:||01 Apr 2008|
|Last Modified:||02 Aug 2016 13:13|
|Share this page:|