The exterior surface of this end piece has a frothy surface and it’s abundantly evident this was a melt that solidified. In between the lobes of the heart tiny studs of metal inclusions slightly protrude. A smoothly crusted surface runs along the top. The cut and polished surface contains a graphite-hued matrix with countless mini-metallic flakes suspended throughout the matrix. Six larger drops of metal are in alignment near the top edge. Other unusual textures add further accents. Impact melt breccias are among the most texturally diverse meteorites as a result of the variables of impact events including the materials doing the impacting, the speed and angle of the projectile, the amount and the flow of the melted target, and the size, shape and abundance of the unmelted inclusions. Modern cutting.
95 x 87 x 25 mm. (3.75 x 3.5 x 1 in.)

263 g. (0.5 lbs.)

While H-melt breccias are extremely rare, the next three lots provide further insight into the rigors to which meteorites are subjected on the part of the Nomenclature Committee of the Meteoritical Society. These three lots do not yet have a name. The scientists on the Nomenclature Committee not only vet the research and determinations made on a new meteorite—they also name it. These three specimens have been confirmed as meteorites and will soon be listed in the Meteoritical Bulletin, but a debate has unfolded as to what to name it. Recovered in the African nation of Niger, these three meteorites are part of the same meteorite shower. As we know exactly where these meteorites were recovered, they should be provided a proper name and not just the name of a collection area followed by a number. The benchmark for providing a proper name, however, requires the substantiation of the circumstances of recovery—and while this information has been provided to the Nomenclature Committee, it is being verified. A name will soon be used to describe the fascinating event from which this meteorite specimen is the heart of the matter.

Christie's would like to thank Dr. Alan E. Rubin at the Institute of Geophysics and Planetary Physics, University of California, Los Angeles for his assistance in preparing this catalogue note.