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Abstract Mineral/melt partition coefficients have been widely used to provide insights into magmatic processes. Olivine is one of the most abundant and important minerals in the lunar mantle and mare basalts. Yet, no systematic olivine/melt partitioning data are available for lunar conditions. We report trace element partition data between host mineral olivine and its melt inclusions in lunar basalts. Equilibrium is evaluated using the Fe-Mg exchange coefficient, leading to the choice of melt inclusion-host olivine pairs in lunar basalts 12040, 12009, 15016, 15647, and 74235. Partition coefficients of 21 elements (Li, Mg, Al, Ca, Ti, V, Cr, Mn, Fe, Co, Y, Zr, Nb, Gd, Tb, Dy, Ho, Er, Tm, Yb, and Lu) were measured. Except for Li, V, and Cr, these elements show no significant difference in olivine-melt partitioning compared to the data for terrestrial samples. The partition coefficient of Li between olivine and melt in some lunar basalts with low Mg# (Mg# < 0.75 in olivine, or < ~0.5 in melt) is higher than published data for terrestrial samples, which is attributed to the dependence of DLi on Mg# and the lack of literature DLi data with low Mg#. The partition coefficient of V in lunar basalts is measured to be 0.17 to 0.74, significantly higher than that in terrestrial basalts (0.003 to 0.21), which can be explained by the lower oxygen fugacity in lunar basalts. The significantly higher DV can explain why V is less enriched in evolved lunar basalts than terrestrial basalts. The partition coefficient of Cr between olivine and basalt melt in the Moon is 0.11 to 0.62, which is lower than those in terrestrial settings by a factor of ~2. This is surprising because previous authors showed that Cr partition coefficient is independent of fO2. A quasi-thermodynamically based model is developed to correlate Cr partition coefficient to olivine and melt composition and fO2. The lower Cr partition coefficient between olivine and basalt in the Moon can lead to more Cr enrichment in the lunar magma ocean, as well as more Cr enrichment in mantle-derived basalts in the Moon. Hence, even though Cr is typically a compatible element in terrestrial basalts, it is moderately incompatible in primitive lunar basalts, with a similar degree of incompatibility as V based on partition coefficients in this work, as also evidenced by the relatively constant V/Cr ratio of 0.039 ± 0.011 in lunar basalts. The confirmation of constant V/Cr ratio is important for constraining concentrations of Cr (slightly volatile and siderophile) and V (slightly siderophile) in the bulk silicate Moon. 

Sr-Nd-Hf-Pb isotopes show that the depleted MORB mantle (DMM) is not homogeneous. The heterogene-ity is attributed to different ages of depletion and/or various degrees of depletion for a given domain of DMM, as well as multiple depletion events, metasomatism, and mixing between DMM and other man-tle components. A mid-ocean ridge basalt, in principle, should contain information about the depletion history of its mantle sources. Here we develop a model to extract the model depletion age and the com-position of a MORB mantle source prior to MORB production using Sr-Nd isotopes or Sr-Hf isotopes in a MORB. The complexities of multiple depletion events, mixing, metasomatism, and enrichment are not addressed in this contribution. The model is based on two assumptions: (i) Isotope evolution in a MORB mantle follows a two-stage evolution model, the first stage in the primitive mantle from the beginning of the solar system to the time of mantle depletion at age Td, and the second stage in the depleted mantle from age Tdto the present day. That is, there is only one single depletion event. The depletion age and degree of depletion of a given mantle source are to be determined. (ii) The trace element composition of a depleted mantle source corresponding to the given MORB can be related to a reference DMM by a log-linear relation with the compatibility index CoI (Zhang, 2014). Applying the two assumptions to the available and large MORB database (Gale et al., 2013), we calculate the global distribution of sub-ridge mantle age and composition. The results show: (i) Mean or reference MORB mantle composition of Salters and Stracke (2004)is close to the average depleted MORB mantle composition, whereas that of Workman and Hart (2005)is significantly more depleted than the average depleted MORB mantle. (ii)Model ages for sub-ridge mantle depletion are mostly between 0.8 to 3.0Ga. (iii) There are large-scale patterns in depletion ages for sub-ridge mantle regions. For example, beneath Mid-Atlantic Ridge, mantle depletion ages are young (0.8 to 2.1 Ga) north of 30◦N, older (1.6 to 4.5 Ga) between 25◦N to 35◦S), and mixed (0.6-4.4 Ga) south of 35◦S. The Pacific sub-ridge mantle has a narrow range of model depletion ages of 1.6 to 3.0 Ga, with a mean of 2.3 Ga. Indian sub-ridge mantle has a younger mean depletion age of 1.7 Ga. These large-scale patterns reveal history of mantle depletion, mantle convection, and possible mixing between older and younger depleted mantles.