Initially, a single, partially fusion-crusted stone weighing 312 g was found in the Northwest Africa desert and purchased through a Moroccan dealer by A. and G. Hupé. The total weight of this material was recorded at 934 g. This meteorite was designated NWA 1877 and classified at the University of Washington in Seattle (A. Irving and S. Kuehner) (see MB #88). A second, larger stone, weighing 642.3 g, was subsequently recovered and purchased through a Moroccan dealer by N. Oakes. This mass, designated NWA 2115, was analyzed at Northern Arizona University (T. Bunch and J. Wittke) and determined to be likely paired with NWA 1877 (see MB #95). This olivine diogenite has been weakly shocked to stage S3 and moderately weathered to grade W2. Additional likely paired fragments have been assigned the names NWA 2286 and NWA 2629 (see MB #89).
Northwest Africa 2115 is a yellow-green harzburgitic peridotite composed primarily of orthopyroxene (up to 11 mm) and large phenocrysts of olivine (up to 18.5 mm) within a disrupted, cataclasized matrix. Minor amounts of chromite (mm-sized), troilite, and virtually Ni-free metal are present. It contains highly-magnesian silicates similar to those in ALHA77256 and GRA 98108. When found, the NWA 1877/2115/2286/2629 masses constituted the fifth representative of the peridotitic olivine diogenite suite of meteorites, which included NWA1459, GRA 98108, ALHA77256, and EETA79002. It has been proposed that this new group, with members containing at least 5% olivine, be called olivine diogenites (A. Irving et al., 2005). Since then, other representative olivine diogenites have been recovered, namely NWA 5405 (~10 vol% olivine), NWA 5312 (24 vol% olivine), NWA 4223 (50 vol% olivine), NWA 5480 (57 vol%), and MIL 07001.
Northwest Africa 2115 contains ~47 vol% olivine with no plagioclase observed, and it has very Cr-rich chromite. Each of these features suggest that NWA 2115 formed at great depth. The higher olivine abundance observed in some of the other olivine diogenites suggests that they were formed in strata at even greater depth, with the features of NWA 5480 possibly indicating an origin as a mantle residue. However, due to the minor and trace element overlaps observed among the diogenite types, they may in fact form a continuum of orthopyroxene accumulation within a fractionated magma ocean or layered intrusion emplaced into the crust. They may represent distinct magma sources rather than each of the olivine diogenites originating in a separate mantle setting (Shearer et al., 2007; 2010).
The dunitic meteorite NWA 2968 (>95 vol% olivine) may be the deepest sampled lithology from the HED parent asteroid, widely thought to be 4 Vesta and its derivitive Vestoids. Notably, Beck et al. (2012) identified the first olivine-rich melt material in howardites that constitute the PCA 02009 pairing group. This olivine-rich material was likely derived from harzburgitic and dunitic lithologies exposed on the surface of Vesta.
It is envisaged by one investigative team that Vesta and the Vestoids, along with the isotopically similar mesosiderites and IIAB irons, were themselves the products of a break-up of an even larger parent object which they have named Opis (Irving et al., 2009). In Greek mythology, Opis was the wife of Saturn, whose children were Jupiter, Neptune, Pluto, Juno, Ceres, and Vesta. Further information about this newly recognized group can be found on the NWA 1459 page. An alternative classification system for the diogenites and dunites based on mineralogical and petrographical features has been proposed by Beck and McSween (2010), and modified by Wittke et al. (2011). The 1.11 g specimen of NWA 2115 shown above is from the 642.3 g main mass, a photo of which is shown below.