¹I. Weber,²U. Böttger,²S. G. Pavlov,^2,3H.-W. Hübers,¹H. Hiesinger,¹E. K. Jessberger
Journal of Raman Spectroscopy 48, 1509-1517 Link to Article [DOI: 10.1002/jrs.5083]
¹Institut für Planetologie, Münster, Germany
²Deutsches Zentrum für Luft- und Raumfahrt (DLR), Institut für Optische Sensorsysteme, Berlin, Germany
³Institut für Optik und Atomare Physik, Humboldt Universität, Institut für Physik, Berlin, Germany

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¹C. Stangarone,²U. Böttger,¹D. Bersani,¹M. Tribaudino,³M. Prencipe
Journal of Raman Spectroscopy 48, 1528-1535 Link to Article [DOI: 10.1002/jrs.5127]
¹Physics and Earth Science Department, University of Parma, Parma, Italy
²Institute of Optical Sensor Systems, DLR, Berlin, Germany
³Earth Science Department, University of Turin, Torino, Italy

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¹Imanol Torre-Fdez,¹Julene Aramendia,¹Leticia Gomez-Nubla,¹Kepa Castro,¹Juan M. Madariaga
Journal of Raman Spectroscopy 48, 1536-1543 Link to Article [DOI: 10.1002/jrs.5148]
¹Department of Analytical Chemistry, Faculty of Science and Technology, University of the Basque Country (UPV/EHU), Bilbao, Spain

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¹Lucie Riu,¹Jean-Pierre Bibring, ¹Cédric Pilorget, ¹François Poulet, ¹Vincent Hamm
Planetary and Space Science (in Press) Link to Article [https://doi.org/10.1016/j.pss.2018.01.009]
¹Institut d’Astrophysique Spatiale, Université Paris-Sud 11, 91405, Orsay, France

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^1,2,3Konstantin D. Litasov, ¹Nikolay M. Podgornykh
Journal of Raman Spectroscopy 48, 1518-1527 Link to Article [DOI: 10.1002/jrs.5119DOI: 10.1002/jrs.5119]
¹V.S. Sobolev Institute of Geology and Mineralogy, Siberian Branch of the Russian Academy of Sciences, Novosibirsk, Russia
²Novosibirsk State University, Novosibirsk, Russia
³Konstantin D. Litasov, V.S. Sobolev Institute of Geology and Mineralogy, Siberian Branch of the Russian Academy of Sciences, Koptyuga Ave., 3, Novosibirsk 630090, Russia.

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¹Punam Dalai, ¹Hannes Lukas Pleyer, ¹Henry Strasdeit, ¹Stefan Fox
Origins of Life and Biospheres 47, 427-452 Link to Article [DOI https://doi.org/10.1007/s11084-016-9523-0]
¹Department of Bioinorganic Chemistry, Institute of Chemistry University of Hohenheim Stuttgart Germany

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¹Ecaterina O. Coman, ¹Bradley L. Jolliff, ¹Paul Carpenter
Icarus (in Press) Link to Article [https://doi.org/10.1016/j.icarus.2018.02.008]
¹Washington University in St. Louis, Saint Louis, MO, 63123, USA
Copyright Elsevier

This paper presents results of coordinated ultraviolet and visible wavelength reflectance measurements, X-ray diffraction analyses of mineral components, and micro X-ray fluorescence analyses of Ti concentrations of 13 lunar soil samples (<210 μm) that span a range of maturity and TiO2 contents. Results of these analyses are used to determine the effects of soil maturity, TiO2 concentration, and specific mineralogical makeup, especially ilmenite content, on the ultraviolet/visible (UV/VIS) ratio for application to remote sensing observations of the Moon and other airless bodies. We find that measured ilmenite weight percent correlates highly with measured TiO2 concentrations. Thus, the ilmenite content is a good predictor of TiO2 concentration. Ilmenite is the main contributor of TiO2 for soils with greater than about 2 weight percent TiO2, so we take the effects of TiO2 on reflectance spectra to be essentially those of ilmenite. Constraining the data set to eight mature Apollo soils, we find that among the UV/VIS ratios from laboratory-measured spectra, the 321/415 nm ratio shows the best correlation with TiO2 and ilmenite. Moreover, for soils with similar maturity in the submature to mature range, those with higher TiO2 have higher 321/415 UV/VIS ratios. Finally, the correlation between TiO2 content and 321/415 ratio in samples measured in the lab appears weaker than for the same relationship using the Lunar Reconnaissance Orbiter (LRO) Wide Angle Camera (WAC) spectral data for the 321/415 ratio of Apollo ground-truth sites. The correlation between lab-derived 321/415 ratios and TiO2 content for measured samples improves when low-maturity samples are excluded from the dataset, implying that the LROC WAC spectra at 400 m/pix spatial resolution senses mostly mature soil.

¹V.A.Alekseev et al. (>10)
Bulletin of the Lebedev Physics Institute 44, 336-339 Link to Article [DOI
https://doi.org/10.3103/S1068335617110069%5D
¹Vernadsky Institute of Geochemistry and Analytical ChemistryRussian Academy of SciencesMoscowRussia

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¹O. Pravdivtseva, ²A.N. Krot, ¹C.M. Hohenberg
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2018.02.004]
¹Physics Department, Washington University, St. Louis MO 63130, USA
²Hawai‘i Institute of Geophysics and Planetology, School of Ocean, Earth Science and Technology, University of Hawai’i at Mānoa, Honolulu, HI 96822, USA
Copyright Elsevier

The I-Xe system was studied in a ferromagnetic sample separated from the Orgueil CI carbonaceous chondrite with a hand-held magnet and in two magnetite samples, one chemically separated before and the other one after neutron irradiation. This work was done in order to investigate the effects of chemical separation by LiCl and NaOH on the I-Xe system in magnetite. Our test demonstrated that the chemical separation of magnetite before irradiation using either LiCl or NaOH, or both, does not contaminate the sample with iodine and thus cannot lead to erroneous I-Xe ages due to introduction of uncorrelated 128∗Xe.

The I-Xe ages of two Orgueil magnetite samples are mutually consistent within experimental uncertainties and, when normalized to an absolute time scale with the reevaluated Shallowater aubrite standard, place the onset of aqueous alteration on the CI parent body at 4564.3 ± 0.3 Ma, 2.9 ± 0.3 Ma after formation of the CV Ca-AI-rich inclusions (CAIs). The I-Xe age of the ferromagnetic Orgueil separate is 3.4 Ma younger, corresponding to a closure of the I-Xe system at 4560.9 ± 0.2 Ma. These and previously published I-Xe data for Orgueil (Hohenberg et al., 2002) indicate that aqueous alteration on the CI parent body lasted for at least 5 Ma.

Although the two magnetite samples gave indistinguishable I-Xe ages, their temperature release profiles differed. One of the two Orgueil magnetites released less radiogenic Xe than the other, 80% of it corresponding to the low-temperature peak of the release profile, compared to only 6% in case of the second Orgueil magnetite sample. This could be due to the difference in iodine trapping efficiencies for magnetite grains of different morphologies. Alternatively, the magnetite grains with the lower radiogenic Xe concentrations may have formed at a later stage of alteration when iodine in an aqueous solution was depleted.

¹Larry R. Nittler, ¹Conel M.O’D. Alexander, ¹Jemma Davidson, ¹My E.I. Riebe,² Rhonda M. Stroud, ¹Jianhua Wang
Geochimica et Cosmochimcia Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2018.01.038https://doi.org/10.1016/j.gca.2018.01.038]
¹Department of Terrestrial Magnetism, Carnegie Institution of Washington, Washington, DC 20015, USA.
²Materials Science and Technology Division, Code 6366, US Naval Research Laboratory, Washington, DC 20375-5320, USA.
Copyright Elsevier

NanoSIMS C-, N-, and O-isotopic mapping of matrix in CO3.0 chondrite Dominion Range (DOM) 08006 revealed it to have in its matrix the highest abundance of presolar O-rich grains (257 +76/-96 ppm, 2σ) of any meteorite. It also has a matrix abundance of presolar SiC of 35 (+25/-17, 2 σ) ppm, similar to that seen across primitive chondrite classes. This provides additional support to bulk isotopic and petrologic evidence that DOM 08006 is the most primitive known CO meteorite. Transmission electron microscopy of five presolar silicate grains revealed one to have a composite mineralogy similar to larger amoeboid olivine aggregates and consistent with equilibrium condensation, two non-stoichiometric amorphous grains and two olivine grains, though one is identified as such solely based on its composition. We also found insoluble organic matter (IOM) to be present primarily as sub-micron inclusions with ranges of C- and N-isotopic anomalies similar to those seen in primitive CR chondrites and interplanetary dust particles. In contrast to other primitive extraterrestrial materials, H isotopic imaging showed normal and homogeneous D/H. Most likely, DOM 08006 and other CO chondrites accreted a similar complement of primitive and isotopically anomalous organic matter to that found in other chondrite classes and IDPs, but the very limited amount of thermal metamorphism experienced by DOM 08006 has caused loss of D-rich organic moieties, while not substantially affecting either the molecular carriers of C and N anomalies or most inorganic phases in the meteorite. One C-rich grain that was highly depleted in 13C and 15N was identified; we propose it originated in the Sun’s parental molecular cloud.