1-s2.0-S0012821X17300353-gr003.sml

Fig. 3. Variation of ratios of Cu, S, Se and Te in Martian meteorites with MgO contents. These element ratios display limited variations for most samples, including different groups of shergottites and nakhlites (except Nakhla). The behavior of the shergottite data differ from the evolution trend of sulfide saturated terrestrial MORB (Jenner and O'Neill, 2012, Lissner et al., 2014) and terrestrial cumulate rocks (Wang and Becker, 2015a), which show strong fractionation of Cu, Se and Te because of different sulfide–silicate melt partition coefficients (Te > Cu > Se ≥ S). S/Se ratios change little during melting and fractional crystallization of basalts, even if sulfide saturation was attained (Jenner and O'Neill, 2012, Wang and Becker, 2015a). Occasionally high S/Se ratios in Martian meteorites (e.g., RBT04262, MIL03346 and LAR06319) reflect assimilation of S from the Martian crust. Blue bands are the ranges of ratios (±1s) in most of the analyzed meteorites (Table 1). Differences between data from the present study and literature data for individual meteorites (Meyer, 2013, Smith et al., 1984, Treiman et al., 1986, Wang et al., 1998; Table S2) are indicated by the dashed line. Error bars (1s) are shown for the new data and most errors are smaller than symbol sizes. (For interpretation of the references to color in this figure legend, the reader is referred to the web version of this article.)