This monomict breccia was found on the Nullarbor Plain of Western Australia by Mrs. J. C. Campbell after she spotted a 503 g specimen from a moving vehicle while travelling cross-country. Eleven additional stones were recovered in July 1985 during a subsequent search of the site, located 200 m west of Camel Donga. Later search parties recovered more stones within the 1 km² area bringing the total known weight to over 2.92 kg.
Camel Donga is a product of fractional crystallization within a magma source and is composed of a mixture of pyroxene and plagioclase in a 3:2 ratio. The fine-grained gray matrix contains gabbroic and doleritic clasts. It contains an unusually high content of total Fe (18.6%), second only to that of NWA 4269 (23.18%). Camel Donga has a high metallic iron content of ~2 wt% (1 vol%) with grain sizes typically ranging from 5 to 10µm and also finely dispersed in silicates. Because of the very low content of Ni (and other siderophile elements) in this metallic iron, it was hypothesized that it formed by in situ reduction of the ferrosilite (FeSiO) component of pyroxene during in situ thermal impact metamorphism (Palme et al., 1988). Data from Hf/W ratios indicate that this thermal metamorphism occurred ~1015 m.y. after mantle differentiation, long after the extinction of the major radiogenic elements. This scenario constrains the cause of the heating event to a major impact on Vesta (Kleine et al., 2004). A similar impact event is thought to have produced the pure Fe-metal in the eucrite NWA 6601 (Agee, 2011).
Conversely, in their study of Camel Donga, Warren and Isa (2015) found a lack of evidence for reduction in either the silicates or the oxides, of which the latter are considered to be the more susceptible to reducing agents. Moreover, they identified a large metal-rich silicate nodule, and other nearby metal aggregates, which have compositions that are enriched in Ni relative to most other Fe-metal phases in the meteorite. It was concluded that this particular metal likely reflects the addition of an impactor component to the material precursive to Camel Donga. In view of these findings, it was proposed that the present composition of Camel Donga (in a similar manner to the eucrite NWA 5738) might reflect episodes of secondary metasomatic alteration by a reducing fluid that originated as a volatile-rich carbonaceous chondrite contaminant.
Camel Donga has an absolute crystallization age based on the PuXe chronometer of 4.507 b.y., and it has a cosmic-ray exposure age of 36.6 (±1.4) m.y., including it within one of the five common breakup events occurring 6 (±2), 12 (±2), 21 (±4), 38 (±8), and 73 (±3) m.y. ago. The pristine condition of these stones is evidence of a recent fall, and it is inferred from their shapes that a single fragmentation was followed by flight orientation of many of the individuals. The occurrence of regmaglypts, radial flow lines, and melt overflow is a common characteristic of many of the stones. The Camel Donga specimen pictured above is a 21.8 g individual with a cut face. The photo below shows the brecciated interior of this eucrite.