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Kimberlites and lamproites were formed in different time; in particular, most
productive kimberlitic magmatism was
observed in the EEP
and SP in the Devonian;
Kimberlite and lamproite bodies have different morphology: lamproites compose small subvolcanic bodies with lava flows, while kimberlites form volcanic pipes with no lavas;
Kimberlites are localized within ancient cratons, while within-plate lamproites are restricted to adjacent Proterozoic belts.
Kimberlites are produced in the low-heat flow
regions, whereas
lamproites
occur in the
high-heat flow
regions;
Kimberlites contain highly silica-undersaturated minerals, while ultrabasic lamproites—silica-undersaturated ones; priderite and wadeite, the characteristic accessory minerals of lamproites, are not observed in kimberlites;
The primary melts of kimberlites and lamproites were derived from different types of mantle. The moderate and low-Ti kimberlites were generated from BSE or EMI type mantle. Precisely these types of kimberlites host diamond deposits, including economic grade objects in EEP. The lamproite sources were localized only in the enriched mantle (EMI and EMII). At the same time, these rocks share some similarities, primarily, with respect to their genesis and classification. Diamonds are common accessory minerals of kimberlites (low-Ti and some other types), but are observed only in only lamproite variety—olivine lamproites.
olivine lamproites
the high-Mg potassic rocks
(kimberlites and lamproites) show
major-component variations, which are significantly wider in lamproites as compared to kimberlites. Kimberlites differ from lamproites not only in the content of SiO2, but also in alkalis, volatiles, and some trace elements. Kimberlites are characterized by CO2-dominated regime, whereas formation
of lamproites was assisted by essentially H2O fluid;