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Oxygen Isotopic Exchange between Amorphous Silicate and Water Vapor and Its Implications for Oxygen Isotopic Evolution in the Early Solar System

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Title: Oxygen Isotopic Exchange between Amorphous Silicate and Water Vapor and Its Implications for Oxygen Isotopic Evolution in the Early Solar System
Authors: Yamamoto, Daiki Browse this author
Kuroda, Minami Browse this author
Tachibana, Shogo Browse this author →KAKEN DB
Sakamoto, Naoya Browse this author
Yurimoto, Hisayoshi Browse this author →KAKEN DB
Keywords: astrochemistry
meteorites, meteors, meteoroids
methods: laboratory: solid state
protoplanetary disks
stars: protostars
Issue Date: 1-Oct-2018
Publisher: IOP Publishing
Journal Title: Astrophysical journal
Volume: 865
Issue: 2
Start Page: 98
Publisher DOI: 10.3847/1538-4357/aadcee
Abstract: Meteoritic evidence suggests that oxygen isotopic exchange between O-16-rich amorphous silicate dust and O-16-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 (m(2) s(-1)) = (1.5 +/- 1.0) x 10(-19) exp[-(161.5 +/- 14.1 (kJ mol(-1))) R-1(1/T-1/1200)] at temperatures below similar to 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 O-16-poor signatures for the most pristine silicate dust observed in cometary materials implies that the cometary silicate dust experienced oxygen isotopic exchange with O-16-poor water vapor through thermal annealing at temperatures higher than 500-600 K prior to their accretion into comets in the solar system.
Rights: https://creativecommons.org/licenses/by/3.0/
Type: article
URI: http://hdl.handle.net/2115/74372
Appears in Collections:理学院・理学研究院 (Graduate School of Science / Faculty of Science) > 雑誌発表論文等 (Peer-reviewed Journal Articles, etc)

Submitter: 圦本 尚義

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