^1,3A.Drouard et al. (>10)
Astronomy & Astrophysics 613, A54 Link to Article [https://doi.org/10.1051/0004-6361/201732225]
¹Aix-Marseille Université, CNRS, LAM (Laboratoire d’Astrophysique de Marseille) UMR 7326, 13388 Marseille, France
²Aix-Marseille Université, CNRS, IRD, Coll France, CEREGE UM34, 13545 Aix en Provence, France

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¹K.Demyk et al. (>10)
Astronomy & Astrophysics 600, A123 Link to Article [https://doi.org/10.1051/0004-6361/201629711]
¹ IRAP, Université de Toulouse, CNRS, UPS IRAP, 9 avenue Colonel Roche, BP 44346, 31028 Toulouse Cedex 4, France

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¹R. de Nutte et al. (>10)
Astronomy & Astrophysics 600, A71 Link to Article [https://doi.org/10.1051/0004-6361/201629195]
¹Institute of Astronomy, KU Leuven, Celestijnenlaan 200D B2401, 3001 Leuven, Belgium
e-mail: rutger.denutte@ster.kuleuven.be

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¹Martin Ferus et al. (>10)
Astronomy & Astrophysics 610, A73 Link to Article [https://doi.org/10.1051/0004-6361/201629950]
¹J. Heyrovský Institute of Physical Chemistry, Academy of Sciences of the Czech Republic, Dolejškova 3, 18223 Prague 8, Czech Republic

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^1,2Quirico, E., ^1,2Bonal, L.
Advances in Astrobiology and Biogeophysics (Book Chapter) Link to Article [DOI: 10.1007/978-3-319-96175-0_2]
¹Université Grenoble Alpes, Grenoble, France
²Institut de Planétologie et d’Astrophysique de Grenoble, Grenoble, France

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¹Erokhin, Y.V., ¹Koroteev, V.A., ¹Khiller, V.V., ¹Ivanov, K.S., ²Kleimenov, D.A.
Doklady Earth Sciences 482, 1189-1192 Link to Article [DOI: 10.1134/S1028334X18090118]
¹Zavaritsky Institute of Geology and Geochemistry, Ural Branch, Russian Academy of Sciences, Yekaterinburg, 620016, Russian Federation
²Ural State Mining University, Yekaterinburg, 620144, Russian Federation

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¹Oshtrakh, M.I., ¹Maksimova, A.A., ¹Goryunov, M.V., ^1,2Petrova, E.V., ³Felner, I., ^1,4Chukin, A.V., ²Grokhovsky, V.I.
Journal of Molecular Structure 1174, 112-121 Link to Article [DOI: 10.1016/j.molstruc.2018.06.039]
¹Department of Experimental Physics, Institute of Physics and Technology, Ural Federal University, Ekaterinburg, 620002, Russian Federation
²Department of Physical Techniques and Devices for Quality Control, Institute of Physics and Technology, Ural Federal University, Ekaterinburg, 620002, Russian Federation
³Racah Institute of Physics, The Hebrew University, Jerusalem, 91904, Israel
⁴Department of Theoretical Physics and Applied Mathematics, Institute of Physics and Technology, Ural Federal University, Ekaterinburg, 620002, Russian Federation

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¹King, A.J., ¹Schofield, P.F., ²Stephen, N.R., ³Frogley, M.D., ³Cinque, G., ¹Russell, S.S.
Infrared Physics and Technology 94, 244-249 Link to Article [DOI: 10.1016/j.infrared.2018.09.020]
¹Planetary Materials Group, Department of Earth Sciences, Natural History Museum, London, SW7 5BD, United Kingdom
²Plymouth Electron Microscopy Centre & School of Geography, Earth and Environmental Sciences, University of Plymouth, Drake Circus, Plymouth, PL4 8AA, United Kingdom
³Diamond Light Source Ltd, Harwell Science Campus, Didcot, OX11 0DQ, United Kingdom

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¹Daiki Yamamoto, ¹Minami Kuroda,^1,2Shogo Tachibana, ³Naoya Sakamoto, ^1,4Hisayoshi Yurimoto
The Astrophysical Journal865, 98 Link to Article [https://doi.org/10.3847/1538-4357/aadcee]
¹Department of Natural History Sciences, Hokkaido University, Sapporo, Hokkaido 060-0810, Japan
²UTokyo Organization for Planetary Space Science, The University of Tokyo, Hongo, Tokyo 113-0033, Japan
³Isotopic Imaging Laboratory, Hokkaido University, Sapporo, 001-0021, Japan
⁴Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency, Sagamihara, Kanagawa, 252-210, Japan

Meteoritic evidence suggests that oxygen isotopic exchange between 16O-rich amorphous silicate dust and 16O-poor water vapor occurred in the early solar system. In this study, we experimentally investigated the kinetics of oxygen isotopic exchange between submicron-sized amorphous forsterite grains and water vapor at protoplanetary disk-like low pressures of water vapor. The isotopic exchange reaction rate is controlled either by diffusive isotopic exchange in the amorphous structure or by the supply of water molecules from the vapor phase. The diffusive oxygen isotopic exchange occurred with a rate constant D (m2 s−1) = (1.5 ± 1.0) × 10−19 exp[−(161.5 ± 14.1 (kJ mol−1))R −1(1/T−1/1200)] at temperatures below ~800–900 K, and the supply of water molecules from the vapor phase could determine the rate of oxygen isotopic exchange at higher temperatures in the protosolar disk. On the other hand, the oxygen isotopic exchange rate dramatically decreases if the crystallization of amorphous forsterite precedes the oxygen isotopic exchange reaction with amorphous forsterite. According to the kinetics for oxygen isotopic exchange in protoplanetary disks, original isotopic compositions of amorphous forsterite dust could be preserved only if the dust was kept at temperatures below 500–600 K in the early solar system. The 16O-poor signatures for the most pristine silicate dust observed in cometary materials implies that the cometary silicate dust experienced oxygen isotopic exchange with 16O-poor water vapor through thermal annealing at temperatures higher than 500–600 K prior to their accretion into comets in the solar system.

¹M. K. Pandey, ^2,3Y. Nishiyama, ^4,5,6P. Tekely
Meteoritics & Planetary Science (in Press) Link to Article [https://doi.org/10.1111/maps.13209]
¹Indian Institute of Technology Ropar, Rupnagar, Punjab, India
²RIKEN CLST‐JEOL Collaboration Center, Yokohama, Kanagawa, Japan
³JEOL Resonance Inc., Akishima, Tokyo, Japan
⁴École Normale Supérieure, Paris, France
⁵Sorbonne Université, Paris, France
⁶CNRS, UMR 7203 Laboratoire des Biomolécules, Paris, France
Published by arrangement with John Wiley & Sons

We recorded one‐ and two‐dimensional solid‐state nuclear magnetic resonance spectra of meteoric insoluble organic matter with unprecedented sensitivity and resolution permitting us to reveal unambiguous spectroscopic fingerprints relevant to its molecular and isotopic features. Two‐dimensional 1H‐1H and 1H‐13C correlation experiments have unveiled the spatial proximity between aliphatic and aromatic groups proving a highly branched character of a rigid macromolecular network composed of short aliphatic chains linking together small aromatic units. One‐dimensional 2H and two‐dimensional 1H‐2H correlation spectroscopy delivered evidence of significant reduction in the deuterium enrichment of aromatic species relevant to interstellar processes, proto‐planetary disk chemistry, and to determining the origin of the meteoritic insoluble organic matter. The experimental approach developed in this work opens new perspectives for systematic and nondestructive analysis at the molecular level of meteoritic insoluble organic matter even with a very small amount of sample from some particularly rare chondrites.