^1,2,3S.F.A. Batista, ^1,3T.M. Seixas, ^1,3M.A. Salgueiro da Silva, ^1,3R.M.G. de Albuquerque
¹Departamento de Física e Astronomia da Faculdade de Ciências da Universidade do Porto, Rua do Campo Alegre, 687, 4169-007 Porto
²Centro de Astrofísica da Universidade do Porto, Rua das Estrelas, 4150-762, Porto
³Centro de Geofísica da Universidade de Coimbra, Av. Dr. Dias da Silva, 3000-134 Coimbra

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Reference
Batista SFA, Seixas TM, Salgueiro da Silva MA, de Albuquerque RMG (2014) Mineralogy of V-type asteroids as a constraining tool of their past history. Planetary&Space Science (in Press)
Link to Article [DOI: 10.1016/j.pss.2014.10.012]

^1,2F. Thiessen, ¹S. Besse, ³M.I. Staid, ⁴H. Hiesinger
¹European Space and Technology Centre, Noordwijk, Netherlands
²Leiden Observatory, Leiden University, Netherlands
³Planetary Science Institute, Tucson, Arizona, USA
⁴Institut für Planetologie, Westfälische Wilhelms-Universität Münster, Germany

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Reference
Thiessen F, Besse S, Staid MI, Hiesinger H (2014) Mapping lunar mare basalt units in mare Imbrium as observed with the moon mineralogy Mapper (M³). Planetary&Space Sciences (in Press)
Link to Article [DOI: 10.1016/j.pss.2014.10.003]

^1,2,3K.T. Howard,⁴C.M.O’D. Alexander, ⁵D.L. Schrader, ⁶K.A. Dyl

¹Kingsborough Community College of the City University of New York. 2001 Oriental Blvd. Brooklyn, NY 11235
²American Museum of Natural History
³The Natural History Museum, London
⁴Department of Terrestrial Magnetism, Carnegie Institution of Washington. 5241 Broad Branch Road, NW Washington, DC 20015-1305
⁵Smithsonian Institution, National Museum of Natural History, Washington. 10th & Constitution NW Washington, DC 20560-0119
⁶Department of Applied Geology, Curtin University of Technology, West Australia, Perth, WA 6845

The relative differences in the degrees of hydration should be reflected in any classification scheme for aqueously altered meteorites. Here we report the bulk mineralogies and degrees of hydration in 37 different carbonaceous chondrites: Renazzo-like (CR), Mighei-like (CM), and ungrouped (type 2) samples. This is achieved by quantifying the modal abundances of all major (phases present in abundances >1wt.%) minerals using Position Sensitive Detector X-ray Diffraction (PSD-XRD). From these modal abundances, a classification scheme is constructed that is based on the normalized fraction of phyllosilicate (View the MathML sourcetotalphyllosilicate/totalanhydroussilicate+totalphyllosilicate). Samples are linearly ranked from type 3.0 – corresponding to a phyllosilicate fraction of <0.05, to type 1.0 – corresponding to a total phyllosilicate fraction of >0.95. Powdered meteorite samples from any hydrated carbonaceous chondrite group can be ranked on this single classification scale. The resulting classifications for CRs exhibit a range from type 2.8 to 1.3, while for CMs the range is 1.7–1.2. The primary manifestation of aqueous alteration is the production of phyllosilicate, which ceased when the fluid supply was exhausted, leading to the preservation of anhydrous silicates in all samples. The variability in hydration indicates that either accretion of ices was heterogeneous or fluid was mobilized. From the bulk mineral abundances of the most hydrated samples, we infer that the initial mass fraction of H2O inside of their parent body(ies) asteroids was <20 wt.%. Bulk carbonaceous chondrite mineralogy evolved towards increasingly oxidizing assemblages as the extent of bulk hydration increased. This is consistent with the escape of reducing H₂ gas that is predicted to have been produced from water during hydration reactions.

Reference
Howard KT, Alexander CMOD, Schrader DL, Dyl KA (2014) Classification of hydrous meteorites (CR, CM and C2 ungrouped) by phyllosilicate fraction: PSD-XRD modal mineralogy and planetesimal Environments. Geochimica et Cosmochimica Acta (in Press) Link to Article [DOI: 10.1016/j.gca.2014.10.025] Copyright Elsevier

¹Ian B. Hutchinson, ¹Richard Ingley, ¹Howell G. M. Edwards, ¹Liam Harris, ¹Melissa McHugh, ^1,2Cedric Malherbe,³J. Parnell
¹Department of Physics and Astronomy, Space Research Centre, University of Leicester, Leicester LE1 7RH, UK
²Department of Inorganic Analytical Chemistry, Chemistry Institute (B6c), University of Liège, 4000 Liège, Belgium
³Department of Geology & Petroleum Geology, University of Aberdeen, King’s College, Aberdeen AB24 3UE, UK

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Reference
Hutchinson IB, Ingley R, Edwards HGM, Harris L, McHugh M, Malherbe C, Parnell J (2014) Research article: Raman spectroscopy on Mars: identification of geological and bio-geological signatures in Martian analogues using miniaturized Raman spectrometers. Philosophical Transactions Royal Society A., 372 20140204
Link to Article [doi:10.1098/rsta.2014.0204]