Syngenetic inclusions in diamond from the Birim field (Ghana) – a deep peridotitic profile with a history of depletion and re-enrichment

Diamonds and their syngenetic mineral inclusions from placer deposits (Akwatia mine) along the Birim River, Ghana were studied, thus providing the first detailed data collection for the West African Craton. Inclusion contents indicate an almost exclusively peridotitic diamond suite, with the vast majority being part of the harzburgitic paragenesis. Chemically the Akwatian diamond inclusions differ from those in our 1100 sample world-wide data base mainly by shifts towards lower Mg/Fe ratios for harzburgitic olivines and orthopyroxenes, extremely high Ni contents in both harzburgitic and lherzolitic olivines, and a higher mean Cr content in chromites. The inconsistency between the low Mg/Fe ratios and the highly refractory compatible trace element signature seems best to be explained by re-fertilisation of a previously depleted source, similar to the metasomatic re-enrichment of deformed, Fe-Ti-rich and hot peridotites discussed by Harte (1983). Geothermometry shows Akwatian inclusions to be 140–190 °C hotter than the peridotitic average (1050 °C) given by Harris (1992). Since garnet-opx equilibria (1100 °C/50 kbar to 1370 °C/67 kbar) indicate a typical shield geotherm (40–42 mW/m²), these elevated temperatures imply an origin of the Akwatian diamonds unusually deep for a peridotitic suite. This is consistent with the presence of extraordinary amounts of silicate spinel component in chromite inclusions, indicative of crystallisation under higher pressures than recorded for most peridotitic suites. In addition, one garnet showed the highest knorringite component (66.4 mol%) so far observed in an inclusion in diamond. The same garnet also contained a minor enstatite solid-solution component, which indicates crystallisation at pressures just below 80 kbar. Akwatian diamond inclusions, therefore, represent the most complete cross-section through peridotitic subcontinental lithospheric upper mantle so far observed, down to a maximum depth between 200–240 km. Received: 1 November 1995 / Accepted 5 January 1997