Fig. 3 (A) Source mixing array for shergottite Lu-Hf and Sm-Nd source compositions calculated using equations of Nyquist et al. (A) Source mixing array.

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Presentation transcript:

Fig. 3 (A) Source mixing array for shergottite Lu-Hf and Sm-Nd source compositions calculated using equations of Nyquist et al. (A) Source mixing array for shergottite Lu-Hf and Sm-Nd source compositions calculated using equations of Nyquist et al. (8) and mantle end-member compositions of Debaille et al. (13). Inset shows a best-fit mixing hyperbola for source Rb/Sr and Sm/Nd compositions of shergottites. Mixing depleted deep mantle (high Lu/Hf, high Sm/Nd, and low Rb/Sr) with 0 to 7% depleted shallower mantle material (low Lu/Hf, high Sm/Nd, and low Rb/Sr) and adding 0.5 to 12% enriched mantle material (low Lu/Hf, low Sm/Nd, and high Rb/Sr) can account for the compositions of depleted, intermediate, and enriched shergottites. NWA 7635 extends the observed range in depleted source compositions for all three isotopic systems. The source composition of ALH 84001 is not used in the regression or modeling but falls within error of the enriched end-member composition in Lu/Hf-Sm/Nd source space and on the mixing hyperbola for Rb/Sr-Sm/Nd source mixtures. Data sources are listed in table S3; ALH 84001 data are obtained from Lapen et al. (12) and Beard et al. (36). (B) Best-fit shergottite mixing line for long- and short-lived Sm-Nd isotope systems with 2σ error envelope. All data, except ALH 84001 and nakhlites (orange), are used in the regression. Average terrestrial standards define zero value for μ142Nd (μ = 100 × ε). DS, depleted shergottites; IS, intermediate shergottites; ES, enriched shergottites. Data sources: black (3), green (11), orange (16), and blue (12). Thomas J. Lapen et al. Sci Adv 2017;3:e1600922 Copyright © 2017, The Authors