A 68 g portion of a stone retaining considerable fusion crust was purchased in Erfoud, Morocco by M. Farmer in October of 2004. A sample was submitted for analysis to Northern Arizona University (T. Bunch and J. Wittke), and NWA 2627 was initially determined to be an anomalous winonaite. The stone has a recrystallized texture and is composed of a heterogeneous mixture of orthopyroxene (44 vol%), olivine (41 vol%), FeS (6 vol%), metallic phases (5 vol%), and plagioclase (3 vol%), along with minor abundances of merrillite, Ca-pyroxene, and chromite.
The mineralogy and composition of this meteorite are similar to those for the lodranites, and when plotted on a diagram comparing the Δ17O-isotopic value vs. Fa mol% in olivine (Rumble III et al, 2005), NWA 2627 clearly lies within the acapulcoite field (see Figure 2 plot in LPSC 38, #2254 ). It has been suggested that this meteorite represents a transitional acapulcoite (Touboul et al., 2007) according to the following classification scheme by Floss (2000) and Patzer et al. (2003) based on metamorphic stage.
primitive acapulcoites: near-chondritic (Se >1213 ppm [degree of sulfide extraction])
typical acapulcoites: FeNiFeS melting and some loss of sulfide (Se ~512 ppm)
transitional acapulcoites: sulfide depletion and some loss of plagioclase (Se <5 ppm)
lodranites: sulfide, metal, and plagioclase depletion (K <200 ppm [degree of plagioclase extraction])
enriched acapulcoites (addition of feldspar-rich melt component)
The high temperatures experienced on the acapulcoite parent body, manifest in the recrystallized texture and occasional partial melt phase, suggest that it accreted very early in Solar System history when radiogenic 26Al was still extant. This was a time period spanning ~13 m.y. after CAI formation, after the accretion of differentiated parent bodies had occurred but before the accretion of chondritic parent bodies had begun (Touboul et al., 2007). However, this formation scenario is inconsistent with some acapulcoites having ages younger than that attributed to the complete extinction of radiogenic 26Al. An impact shock heating model has been proposed by Rubin (2007), the details of which can be found on the Monument Draw page.
Data for cooling rates indicate a more rapid cooling for the acapulcoite parent body than that which the bulk H chondrite parent body experienced (but similar to that of H4 chondrites; Kleine et al., 2007), consistent with a smaller acapulcoite parent body and/or a near-surface residence for the acapulcoites. The possibility also exists for a collisional disruption early in its history, forming sub-km- to multi-km-sized fragments, which eventually succumbed to gravitational reassembly. Compared to the lodranite lithological unit, both the primitive and typical acapulcoites are thought to have originated in the outermost layer of the asteroid where cooling began earlier and at a faster rate consistent with the older gas retention ages, finer-grain size, and less intense metamorphism (<13% silicate partial melting) for those meteorites. The lodranites experienced higher degrees of FeNiFeS melting as well as silicate partial melting (~520%), with loss of an FeS and a basaltic component. The transitional acapulcoites exhibit features (e.g., HSE-rich metal) consistent with extensive melting of metal and sulfide phases including melt migration and pooling, representing a continuum between the formation of acapulcoites and lodranites, or alternatively, representing formation at greater depths associated with core formation (Dhaliwal et al., 2017). For more complete and current formation scenarios of the acapulcoitelodranite parent body see the Lodran page.
Northwest Africa 2627 has been weathered to grade W2/3 and has been shocked to stage S2. The 210 g acapulcoite NWA 4399 might be paired. The photo of NWA 2627 shown above is a 0.88 g partial slice, photographed by Jim Strope.