Introduction: Martian (SNC) meteorites are igneous rocks from young (except for ALH 84001, which is much older), thick lava flows or shallow intrusions [1]. The shergottites (‘S’ of SNC) can be categorized according to LREE depletion into highly, moderately, and slightly depleted groups [1]. The La/Lu ratio (and other depletion indicators) is positively correlated with oxygen fugacity, and this...

available online at http://meteoritics.org 1175 © The Meteoritical Society, 2005. Printed in USA. Petrology, geochemistry, and cosmic-ray exposure age of lherzolitic shergottite Northwest Africa 1950 P. GILLET1*, J. A. BARRAT2, P. BECK1, B. MARTY3, R. C. GREENWOOD4, I. A. FRANCHI4, M. BOHN5, and J. COTTEN6 1Laboratoire des Sciences de la Terre, CNRS UMR 5570, Ecole Normale Supérieure de Lyon, 4...

Introduction: Phosphate minerals are thought to occur in chondritic parent bodies mainly as a result of secondary alteration processes [1]. Jones et al., [2] investigated the textural occurrences of phosphates in a range of Ordinary Chondrites (OCs) (petrologic types 3.9–6) and found support for a model involving progressive solid-state recrystallisation and equilibration in a closed parent bod...

Introduction: We present a spectral deconvolution technique and model based on the description of electronic transition absorption bands in continuumremoved spectra. The model differs from the standard gaussian modeling in the way the continuum is removed. An improved nonlinear curve fitting algorithm is used to fit the model to the data. The approach represents also an alternative to the MGM m...

The physical state of silica is a very useful index of shock in meteorites. Its study has been revived by the discovery of high pressure silica in Shergotty of the αPbO2 and ZrO2 structure [14]. Shergottites usually contain a few percent of silica with varied textures depending on their location in the rock. Cathodoluminescence (CL) imaging and spectroscopy is a powerful technique which enables...

Introduction: EETA 79001 is a particularly interesting martian meteorite because the impact melts in it contain noble gas signatures indicative of martian origin [1]. The noble gases were initially thought to be from martian atmosphere [1] and later revised to be from martian aqueous solution [2]. In either scenario, the impact melts acquired the noble gases could also have acquired martian H2O...

Introduction: Mineral equilibria provide predic-tors of properties important in aqueous geochemistry (solubility, freezing, precipitation, dissolution, etc.). Prediction works well where groundwater is well above freezing, but less so where only thin films of cold water and ice are present. Calculations are also limited where water/rock ratios are small, the general case on Mars. On Mars many m...

Introduction: Martian meteorites (MM) comprise rocks shocked in the range of 5-55 GPa during natural impact events [1]. Together with the suite of experimentally shocked rocks, they are valuable assets for the study of the progressive stages of shock metamorphism. Petrographic investigations of MM, in combination with shock and post shock temperature calculations are presented. This data set is...

1753. 38th LPSC. 5031 THE ASSEMBLAGE NATIVE COPPER, COBALTIAN KAMACITE, AND TROILITE IN ORDINARY CHONDRITES: DISSOCIATION PRODUCTS NOT RELATED TO A SHOCK EVENT H. Chennaoui Aoudjehane1, A. El Goresy2, and A. Jambon3. 1Universite Hassan II Aln Chock, Laboratoire Geosciences, BP 5366 MaarifCasablanca, Morocco. E-mail: [email protected]. 2Bayerisches Geoinstitut, UniversiUit Bayreuth, 95447 B...

Introduction: The lunar meteorites Miller Range 05035 (MIL) and Meteorite Hills 01210 (MET) were collected during the 2005 and 2001 ANSMET (Antarctic Meteorite Search) field seasons [1,2]. MET is a 22.8 g regolith breccia composed primarily of basaltic material [3-6]. MIL is a 142.2 g coarse-grained basalt [2]. The bulk composition, mineral assemblage, and texture of MIL is similar to lunar met...