1Ray D.,1Baliyan S.,2Nayak C.
Advances in Space Research 68, 3233-321 Link to Article [DOI 10.1016/j.asr.2021.06.009]
1Planetary Sciences Division, Physical Research Laboratory, Ahmedabad, 380 009, India
2Atomic & Molecular Physics Division, Bhabha Atomic Research Centre, Mumbai, 400085, India
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1Tiwari K.,1Ghosh S.,2Miyahara M.,3Ray D.
Geophysical Research Letters 48, e2021GL093592 Link to Article [DOI 10.1029/2021GL093592]
1Department of Geology and Geophysics, Indian Institute of Technology Kharagpur, Kharagpur, India
2Graduate School of Advanced Science and Engineering, Hiroshima University, Hiroshima, Japan
3Planetary Sciences Division, Physical Research Laboratory, Ahmedabad, India
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1Mason Neuman,1,2Astrid Holzheid,1Katharina Lodders,1Bruce FegleyJr.,1Bradley L.Jolliff,1Piers Koefoed,3Heng Chen,1Kun Wang王昆
Geochimica et Cosmochimica Acta (in Press) Link to Article [https://doi.org/10.1016/j.gca.2021.09.035]
1Department of Earth and Planetary Sciences and McDonnell Center for the Space Sciences, Washington University in St. Louis, One Brookings Drive, St. Louis, MO 63130, USA
2Institute of Geosciences, Kiel University, 24098 Kiel, Germany
3Lamont-Doherty Earth Observatory, Columbia University, Palisades, NY 10964, USA
Copyright Elsevier
The chemical and isotopic signatures of moderately volatile elements are useful for understanding processes of volatile depletion in planetary formation and differentiation. However, the fractionation factors between gas and melt phases during evaporation that are required to model these planetary volatile depletion processes are still sparse. In this study, twenty heating experiments were conducted in 1 atm gas-mixing furnaces to constrain the behavior of K, Cu, and Zn evaporation and isotopic fractionation from basaltic melts at high temperatures. The temperatures range from 1300 °C to 1400 °C, and durations are from 2 to 8 days. Oxygen fugacities (fO2) range from one log unit below to ten log units above that of the iron-wüstite buffer (IW–1 to IW+10, corresponding to logfO2 of –10.7 to –0.68 at 1400 °C). The conditions were selected to achieve an evaporation-dominated regime (where timescales of diffusion << evaporation for trace elements) in order to avoid diffusion-limited evaporation. Our results show during evaporation Zn behaved as the most volatile, followed by Cu and then K, regardless of temperature and oxygen fugacity. Partitioning of Zn into spinel layers within experimental capsules, however, has been observed, which has substantial effects on the Zn isotope fractionation factor. Therefore, Zn results are presented but further discussion is excluded. Element loss depends on both temperature and oxygen fugacity, where higher temperatures and lower oxygen fugacities promote evaporation. However, with varying temperature and oxygen fugacity, the kinetic isotopic fractionation factors, α (where, RR0=fα-1), for K and Cu remain constant, thus these factors can be applied to a wider range of conditions than those in this study. The experimentally determined fractionation factors for K, and Cu during evaporation from basaltic melts are 0.9944, and 0.9961, respectively. The fractionation factors for these elements with varying volatilities are all significantly larger than the “apparent observed fractionation factors,” which approach one and are inferred from lunar basalts relative to the Bulk Silicate Earth. This observation suggests near-equilibrium conditions during volatile-element loss from the Moon as the “apparent observed fractionation factors” of lunar basalts are similar for all three elements.
Cosmochemistry Papers 