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Edited by Mark H. Thiemens, University of California, San Diego, La Jolla, CA, and approved July 14, 2017 (received for review May 18, 2017)
Article Figures & SI
Figures
- Fig. 1.
Values of δ68Zn versus δ66Zn for components in Apollo 66095 and 14053, and for previously published mare basalt, FAN, high-Mg suite (HMS), and lunar volcanic beads, 74220 and 15426 (3, 4). Dashed lines denote zero values, and solid line denotes regression through 66095 and 14053 data, collected during the same analytical campaign (slope of 2.0037; R2 = 0.9999).
- Fig. 2.
Chlorine versus Zn isotopic evolution in a progressively crystallizing magma ocean at different fractionation factors for Cl (α = 0.9995 to 0.993). Preferential retention of Zn due to olivine melt partitioning of ∼1, compared with <1 for Cl (and Pb) leads to rapid depletion in Pb and Cl in the Moon, even with an α fractionation of 0.9995. The isotopically heavy Cl, high U/Pb, and moderately positive δ66Zn therefore reflects different preservation of moderately volatile elements in a crystallizing Moon. Volatile loss would commence with the earliest and most volatile-rich magma ocean cumulates (stage a), to crust formation (stage b), followed by late-stage intrusion, Fe−Ti oxide overturn, and mare basalt magmatism (stage c). The starting composition for lunar evolution is assumed to be identical to that of the bulk silicate Earth in this model (δ37Cl = ∼0‰; δ66Zn = ∼0.3‰). High-Ti, high-Ti mare basalts; HMS, high-Mg suite; Low Ti, low-Ti mare basalts; LVB, lunar volcanic beads.
- Fig. 3.
Zinc concentration versus δ66Zn in (A) leaches and residues of Apollo mare basalt 14053 versus published data for low-Ti and high-Ti mare basalts and (B) for 66095, FANs, high-Mg suite and high-alkali suite (HMS/HAS) rocks, lunar volcanic beads (15426, 74220) and mare basalts filtered for condensate Zn addition (values less than chondritic δ66Zn). Models show simple mixing between average mare basalt and 66095 compositions (i) and 10:1 addition of a sulfidic condensate component to pristine FAN (ii). Gray lines are the terrestrial and chondritic average δ66Zn from ref. 3. Data sources are as for Fig. 1, with analytical errors being smaller than symbols.
Data supplements
Volatile-depleted Moon
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