Different types of CaSiO3 in the Earth’s mantle and its geochemical heterogeneity: the Juina area in Brazil as an example

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CaSiO3 inclusions in diamonds from the Juina area in Brazil have low Fe (0.08–0.53 wt. % FeO) and Al (0–1.52 wt. % Al2O3) concentrations; they belong to the ultramafic association. Two different types exist among CaSiO3 grains. Type I has a normal REEn pattern, while type II has a sinusoidal REEn pattern. Type I CaSiO3 associates with high-Mg – high-Ni protogenetic ferropericlase, and type II associates with high-Fe – low-Ni syngenetic ferropericlase. Thus, type I CaSiO3 grains are protogenetic, formed, like high-Mg – high-Ni ferropericlase, in the upper part of the lower mantle as davemaoite (CaSi-perovskite), and type II CaSiO3 were formed in the transition zone as breyite. The enrichment of CaSiO3 in REE, particularly in LREE, corresponds to high values of their partition coefficient CaSiO3/melt and shows the Ca-SiO3’s origin from a mantle material under high pressures. The isotope characteristics of the studied CaSiO3 demonstrate strong geochemical heterogeneity in the inclusions. The 87Rb/86Sr ratios in type II CaSiO3 (0.127–3.23) are 3–4 orders higher than in type I (0.0008). Even within a single diamond, different CaSiO3 grains have 87Rb/86Sr ratios varying from 0.014 to 3.23. The same is true for U/Pb isotope systematics (e. g., 238U/206Pb varies in one sample in an order of magnitude from 0.031 to 0.312) and, to some extent, for Sm/Nd ratios. This implies the geo-chemical heterogeneity in Deep Earth on a very small scale.

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F. Kaminsky

Vernadsky Institute of Geochemistry and Analytical Chemistry, Russian Academy of Sciences

编辑信件的主要联系方式.
Email: kaminsky@geokhi.ru
ORCID iD: 0000-0001-6035-7114
俄罗斯联邦, Kosygin Str., 19, Moscow, 119991

Yu. Kostitsyn

Vernadsky Institute of Geochemistry and Analytical Chemistry, Russian Academy of Sciences

Email: kaminsky@geokhi.ru
俄罗斯联邦, Kosygin Str., 19, Moscow, 119991

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2. Fig. 1. The Juina diamondiferous district and the location of the Rio Sorriso placer (red star). Modified from Kaminsky et al. (2010).

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3. Fig. 2. Position of the Juina region (red star) in the Amazon Craton. Modified from Cordani and Teixeira (2007).

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4. Fig. 3. Ages of inclusions in diamonds from the Juina area. Data from Bulanova et al. (2010), Hutchison et al. (2012), Smit et al. (2022), Nestola et al. (2023), Timmerman et al. (2023).

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5. Fig. 4. CaSiO3 inclusions exposed on the polished surface of diamonds. After Timmerman et al. (2023). © Nature.

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6. Fig. 5. Chemical compositions of CaSiO3 inclusions of ultramafic and mafic parageneses. All four studied CaSiO3 inclusions from the Rio Sorriso placer (shown with asterisks) belong to the ultramafic paragenesis. Based on (Kaminsky, 2017, Fig. 5.5a).

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7. Fig. 6. Chondrite-normalized REE distribution in CaSiO3 included in diamonds from the Rio Sorriso placer. The shaded green area shows REE variations in sample #2.2.3. The thin gray line shows the REE distribution between CaSiO3-perovskite and melt after Corgne et al. (2005). Analytical data after Timmerman et al. (2023). Chondrite data after McDonough, Sun (1995). Data for the Machado sample after Burnham et al. (2016).

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8. Fig. 7. Ratio of medium and heavy with light REE in the studied CaSiO3 samples. Data source – Table 2. The red star corresponds to the chondrite composition according to McDonough, Sun (1995).

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9. Fig. 8. Rb–Sr (a), Sm–Nd (b), and Pb (c) isotopic data for the studied CaSiO3 inclusions in diamonds from the Juina area. MORB and OIB data from Kostitsyn (2004, 2007). For comparison, Figs. (a) and (b) also show the lines corresponding to the age of the Juina pipe – 90 Ma. The analytical points do not fall on this line or on any other.

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