Source regions of carbonaceous meteorites and near-Earth objects

Abstract

Context . The source regions of ordinary chondrites (~80% of all falls) and large S-type near-Earth objects (NEOs; ~30%) have recently been identified with three young asteroid families (Karin, Koronis, Massalia) being at the origin of most ordinary chondrite falls. Aims . The present work is a continuation of our previous studies and aims to determine the source regions of the remaining meteorite and NEO classes, with an emphasis on carbonaceous chondrites (CM, CI, CO, CV, CK, CR, CH, CB, or C-ungrouped). Methods . We studied 38 individual asteroid families, including young and old ones, and determined their contributions to the NEO populations at metre and kilometre sizes using collisional and orbital models. Our models are in agreement with spectroscopic observations of NEOs, cosmic-ray exposure ages of meteorites, statistics of bolides, infrared emission from dust bands, composition of interplanetary dust particles (IDPs), and abundance of extraterrestrial helium-3. Results . We identified the Veritas, Polana, and Eos families as the primary sources of CM/CR, CI, and CO/CV/CK chondrites, respectively. Substantial contributions are also expected from CM-like König and CI-like Clarissa, Misa, and Hoffmeister families. The source regions of kilometre-sized bodies are generally different. The Adeona family is by far the main source of CM-like NEOs, whereas the Polana (low-i) and Euphrosyne (high-i) families are at the origin of most CI-like NEOs. The Polana family is the likely source of both Ryugu and Bennu. We were able to link spectroscopically and dynamically several NEOs to the Baptistina family. Finally, it appears that the pre-atmospheric flux of carbonaceous chondrites at metre sizes is about the same as that of ordinary chondrites. Given the difference in fall statistics between the two groups (80% versus 4.4%), this implies either substantial atmospheric fragmentation of carbonaceous bodies at the level of ~0.5 MPa or destruction by thermal cracking and water desorption. Conclusions . The source regions of most meteorites and kilometre-sized NEOs have now been determined, including some minor classes such as enstatite chondrites and achondrites (Nysa, Hungaria), acapulcoites and lodranites (Iannini). Future work should focus on the few remaining classes (essentially, iron meteorites, pallasites, and ureilites).