HED meteorites are a clan (subgroup) ofachondrite meteorites. HED stands for "howardite–eucrite–diogenite".These achondrites came from adifferentiated parent body and experienced extensive igneous processing not much different from the magmatic rocks found on Earth and for this reason they closely resemble terrestrial igneous rocks.[1]
No matter their composition, all these types of meteorite are thought to have originated in the crust of the asteroidVesta.[6][7] According to this theory, the differences of composition are due to their ejection at different moments in the geologic history of Vesta. Their crystallization ages have been determined to be between 4.43 and 4.55 billion years fromradioisotope ratios. HED meteorites aredifferentiated meteorites, which were created by igneous processes in the crust of their parent asteroid.
It is thought that the method of transport from Vesta toEarth is as follows:[8]
An impact on Vesta ejected debris, creating small (10 kilometres (6.2 mi)diameter or less)V-type asteroids. Either the asteroidal chunks were ejected as such, or were formed from smaller debris. Some of these small asteroids formed theVesta family, while others were scattered somewhat further.[9] This event is thought to have happened less than 1 billion years ago.[10] There is an enormous impact crater on Vesta covering much of the southern hemisphere which is the best candidate for the site of this impact. The amount of rock that was excavated there is many times more than enough to account for all known V-type asteroids.
Some of the more far-flung asteroid debris ended up in the 3:1Kirkwood gap. This is an unstable region due to strong perturbations byJupiter, and asteroids that end up here get ejected into very different orbits on a timescale of about 100 million years. Some of these bodies are perturbed into near-Earth orbits forming the small V-typenear-Earth asteroids such as e.g.3551 Verenia,3908 Nyx, or4055 Magellan.
Later, smaller impacts on these near-Earth objects dislodged rock-sized meteorites, some of which later struck Earth. On the basis ofcosmic ray exposure measurements, it is thought that most HED meteorites arose from several distinct impact events of this kind, and spent from about 6 million to 73 million years in space before striking the Earth.[11]
^McSween, H. Y.; R. P. Binzel; M. C. De Sanctis; E. Ammannito; T. H. Prettyman; A. W. Beck; V. Reddy; L. Le Corre; M. J. Gaffey; et al. (27 November 2013). "Dawn; the Vesta-HED connection; and the geologic context for eucrite, diogenites, and howardites".Meteoritics & Planetary Science.48 (11): 2090–21–4.Bibcode:2013M&PS...48.2090M.doi:10.1111/maps.12108.
^Eugster, O.; Michel, Th. (1995). "Common asteroid break-up events of eucrites, diogenites, and howardites, and cosmic-ray production rates for noble gases in achondrites".Geochimica et Cosmochimica Acta.59 (1):177–199.Bibcode:1995GeCoA..59..177E.doi:10.1016/0016-7037(94)00327-I.
