Interplanetary dust, micrometeorites, and meteorites should share some common physical and chemical properties if the small dust particles as well as the larger extraterrestrial samples originate in the asteroid belt. Indeed, interplanetary dust particles (IDPs) and micrometeorites were found showing clear relationships to existing meteorite classes and to specific components of carbonaceous chondrites. Primitive anhydrous IDPs, though mineralogically unlike known meteorites, contain forsterite with a unique chemical signature which are also present in primitive chondrites, and therefore establish a link between IDPs and meteorites. These primitive anhydrous IDPs are most likely derived from objects in the asteroid belt which do not deliver meteorites to Earth. A number of IDPs appear to be samples of strongly heated or melted parent bodies and could establish links to Acapulcoites and the even more reduced silicates in type IAB iron meteorites. Refractory IDPs with isotopic and chemical properties of Calcium‐Aluminum‐Rich Inclusions (CAIs) are present among stratospheric dust particles. They suggest a relationship of some IDPs with carbonaceous chondrites, although a small number of CAIs are also reported from ordinary chondrites. However, IDPs mineralogically identical to equilibrated ordinary chondrites have not so far been identified. It is therefore most likely that refractory IDPs are samples from similar to carbonaceous chondrite parent bodies.
Among Antarctic micrometeorites is a sizable population of unmelted particles. These unmelted micrometeorites are most likely the products of thermally altered hydrous phases. This population of micrometeorites, originating from aqueously altered parent objects in the asteroid belt, is comparable in abundance to the hydrated class of IDPs among stratospheric dust particles. The majority of hydrated IDPs are however not identical to the known aqueously altered meteorites. One micrometeorite from Antarctica, having its phyllosilicates preserved, establishes a link between unmelted micrometeorites and smectite‐type IDPs. A number of aqueously altered parent objects in the asteroid belt could account for the existence of abundant hydrated particles among IDPs and micrometeorites. These hydrous asteroids are however not sampled by the known meteorites.
