Ordinary chondrites are the most common type of chondrites. As a non-destructive, rapid, and semi-quantitative technology, Raman spectroscopy is widely used in geoscience. This paper presents results spectroscopic study that we conducted for 16 ordinary with different chemical groups variable degrees shock metamorphism. We found that: (1) relationship between Fe composition olivine pyroxene cha...

High-pressure Raman spectroscopy was used to follow the effects of a phase transition on the Raman spectrum of a natural specimen of the pyroxene spodumene, from its low-pressure (C2/c) to its highpressure (P21/c) phases. The transition occurred at 3.2 GPa and was accompanied by an increase from 15 to 23 observed peaks, owing to a decrease in symmetry. Comparisons were made with other pyroxenes...

Introduction: Because they are dominated by enstatite, a nearly FeO-free pyroxene, and Si-bearing FeNi metal, along with minor amounts of unusual monosulfides such as niningerite (MgS), oldhamite (CaS) and alabandite (MnS), the enstatite chondrites have long been thought to have formed under extremely reducing conditions [1,2]. Like the ordinary chondrites, enstatite chondrites exhibit a range ...

available online at http://meteoritics.org Characterization of the 1.2 μm M1 pyroxene band: Extracting cooling history from near-IR spectra of pyroxenes and pyroxene-dominated rocks Rachel L. KLIMA1*, Carlé M. PIETERS1, and M. Darby DYAR2 1Department of Geological Sciences, Brown University, Providence, Rhode Island 02906, USA 2Department of Astronomy, Mount Holyoke College, South Hadley, Massa...

Introduction: We have studied the petrography and Fe-isotope composition of seven chondrules, four from the Allende (CV3) carbonaceous chondrite and three from the Chainpur (LL3.4) ordinary chondrite. Three textural-chemical chondrule types are represented within this sample set: (1) BO, (2) RP and (3) PO/POP. These textural differences allow us to exa mine the Fe-isotope composition in materia...

We present the thermal infrared (5–35 lm) spectrum of 956 Elisa as measured by the Spitzer Infrared Spectrograph (‘‘IRS’’; Houck, J.R. et al. [2004]. Astrophys. J. Suppl. 154, 18–24) together with new groundbased lightcurve data and near-IR spectra. From the visible lightcurve photometry, we determine a rotation period of 16.494 ± 0.001 h, identify the rotational phase of the Spitzer observatio...