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[1] Abyssal peridotites, the depleted solid residues of ocean ridge melting, are the most direct samples available to assess upper oceanic mantle composition. We present detailed isotope and trace element analyses of pyroxene mineral separates from Southwest Indian Ridge abyssal peridotites and pyroxenites in order to constrain the size and length scale of mantle heterogeneity. Our results demonstrate that the mantle can be highly heterogeneous to <1 km and even <0.1 m length scales. Examination of Nd isotopes in relation to modal, trace, and major element compositions indicate that the length scales and amplitudes of heterogeneities in abyssal peridotites reflect both ancient mantle heterogeneity and recent modification by melting, melt-rock reaction and melt crystallization. The isotopic and trace element compositions of pyroxenite veins in this study indicate that they are not direct remnants of recycled oceanic crust, but instead are formed by recent melt crystallization. Combined with existing data sets, the results show that the average global isotopic composition of peridotites is similar to that of mid-ocean ridge basalts, though peridotites extend to significantly more depleted 143 Nd/ 144 Nd and 87 Sr/ 86 Sr. Standard isotope evolution models of upper mantle composition do not predict the full isotopic range observed among abyssal peridotites, as they do not account adequately for the complexities of ancient and recent melting processes.

A method for the determination of major, minor and trace elements in silicate samples by ICP‐QMS and ICP‐SFMS applying isotope dilution‐internal standardisation (ID‐IS) and multi‐stage internal standardisation has been developed. Samples with an enriched isotope of 149Sm (spike) were decomposed by a HF/HCIO4 mixture and stepwise drying and finally diluted. In ID‐IS for trace element analyses by Q‐pole type ICP‐MS (ICP‐QMS), the Sm concentration was determined by ID, while other trace elements (Li, Be, Rb, Sr, Y, In, Cs, Ba, La, Ce, Pr, Nd, Eu, Gd, Tb, Dy, Ho, Er, Tm, Yb, Lu, Tl, Pb, Bi, Th and U) were determined using the 149Sm intensity as an internal standard. Major and minor elements were determined by multi‐stage internal standardisation, with Na, Mg, Al, P, Ca, V, Mn, Fe and Co measured by sector magnetic field type ICP‐MS (ICP‐SFMS) at middle resolution (MR; M/AM =∼ 3000) using Sr determined by ICP‐QMS in the sample as the internal standard. Potassium, Sc, Ni, Cu, Zn and Ga were measured at high resolution (HR; M/ΔM ∼ 7500) using the Sr concentration obtained by ICP‐QMS or the Mn concentration obtained by ICP‐SFMS at MR as internal standard. The merit of ID‐IS is that accurate dilution of the sample is not required. Matrix effects on elemental ratios down to a dilution factor (DF) of 600 were not observed in either types of mass spectrometry. Pseudo‐flow injection (FI), where transient signals were integrated, was used in ICP‐QMS, while conventional continuous sample introduction was used in ICP‐SFMS, resulting in total required sample solutions of 0.026 ml and 0.08 ml, respectively. Detection limits were low enough to determine these elements in depleted ultramafic rocks, and typical reproducibilities for basalts were 3% (Li‐Be), 1% (Rb‐U), 5% (In, Tl and Bi), 7% (Sc‐Ga) and 3% (major elements). Carbonaceous chondrites including Orgueil (Cll), Murchison (CM2) and Allende (CV3), as well as reference materials, JB‐1, ‐2, ‐3, JA‐1, ‐2, ‐3 and JP‐1 (GSJ), BHVO‐1, AGV‐1, PCC‐1 and DTS‐1 (USGS), were analysed to show the applicability of this method. Une méthode permettant la détermination des éléments majeurs, mineurs et en trace dans les echantillons silicates par ICP‐QMS et ICP‐SFMS a été développée. Elle combine la standardisation interne par dilution isotopique (ID‐IS) et la standardisation interne en deux étapes. Les échantillons, auxquels est ajouté un spike enrichi en 149 Sm, sont décomposés par une mixture HF/HCIO4′ séchés progressivement puis dilués. Dans la phase de standardisation interne par dilution isotopique avec un ICP‐MS à quadrupôle (ICP‐QMS), la concentration en Sm est déterminée par dilution isotopique tandis que les autres éléments en trace (Li, Be, Rb, Sr, Y, In, Cs, Ba, La, Ce, Pr, Nd, Eu, Gd, Tb, Dy, Ho, Er, Tm, Yb, Lu, Tl, Pb, Bi, Th et U) sont déterminés en utilisant le signal de 149 Sm comme standard interne. Les éléments majeurs et mineurs sont déterminés par standardisation interne par étapes, avec Na, Mg, Al, P, Ca, V, Mn, Fe et Co mesurés par ICP‐MS à secteur magnétique (ICP‐SFMS...

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C-type asteroids1 are considered to be primitive small Solar System bodies enriched in water and organics, providing clues to the origin and evolution of the Solar System and the building blocks of life. C-type asteroid 162173 Ryugu has been characterized by remote sensing2–7 and on-asteroid measurements8,9 with Hayabusa2 (ref. 10). However, the ground truth provided by laboratory analysis of returned samples is invaluable to determine the fine properties of asteroids and other planetary bodies. We report preliminary results of analyses on returned samples from Ryugu of the particle size distribution, density and porosity, spectral properties and textural properties, and the results of a search for Ca–Al-rich inclusions (CAIs) and chondrules. The bulk sample mainly consists of rugged and smooth particles of millimetre to submillimetre size, confirming that the physical and chemical properties were not altered during the return from the asteroid. The power index of its size distribution is shallower than that of the surface boulder observed on Ryugu11, indicating differences in the returned Ryugu samples. The average of the estimated bulk densities of Ryugu sample particles is 1,282 ± 231 kg m−3, which is lower than that of meteorites12, suggesting a high microporosity down to the millimetre scale, extending centimetre-scale estimates from thermal measurements5,9. The extremely dark optical to near-infrared reflectance and spectral profile with weak absorptions at 2.7 and 3.4 μm imply a carbonaceous composition with indigenous aqueous alteration, matching the global average of Ryugu3,4 and confirming that the sample is representative of the asteroid. Together with the absence of submillimetre CAIs and chondrules, these features indicate that Ryugu is most similar to CI chondrites but has lower albedo, higher porosity and more fragile characteristics.