A cv chondrite clast in a ck chondrite?

Introduction: The physical evolution of asteroids is driven by multiple episodes of collisional processes, such as excavation of materials, mixing, and reaccretion [e.g., 1]. Brecciated meteorites and meteorites containing xenolithic clasts provide evidence of these dynamic impact-dominated parent body histories. Though the number of meteorites containing foreign clasts is not well constrained, brecciation is common among many groups of meteorites (e.g., CI, CM, and CV carbonaceous chondrites, aubrites, mesosiderites, and HEDs) [1]. In fact, a recent study by [2] suggests that 27% of ordinary chondrites the largest group of meteorites are breccias. Recently, we purchased a 4 g slice of Northwest Africa (NWA) 11241, which was initially classified as a CV chondrite. This sample contains an ~8 x 5 mm chondritic clast (Fig. 1). The boundary between the clast and the host meteorite is very sharp, and the clast is texturally distinct from the host, suggesting that the clast and the host meteorite represent material from two parent asteroids. Here, we characterize the texture and mineralogy of the chondritic clast in order to determine its parent body. We also reexamine the initial classification of NWA 11241, as it is petrographically similar to the CK chondrites.