A Southwest Research Institute-led team of scientists has identified a potentially new meteorite parent asteroid by studying a small shard of a meteorite that arrived on Earth a dozen years ago. The composition of a piece of the meteorite Almahata Sitta (AhS) indicates that its parent body was an asteroid roughly the size of Ceres, the largest object in the main asteroid belt, and formed in the presence of water under intermediate temperatures and pressures.
Asteroids — and the meteors and meteorites that sometimes come from them — are leftovers from the formation of our Solar System 4.6 billion years ago. Most reside in the main asteroid belt between the orbits of Mars and Jupiter, but collisions and other events have broken them up and ejected remnants into the inner Solar System. In 2008, a 9-ton, 13-foot diameter asteroid entered Earth’s atmosphere, exploding into some 600 meteorites over the Sudan. This marked the first time scientists predicted an asteroid impact prior to entry and allowed recovery of 23 pounds of samples.
“We were allocated a 50-milligram sample of AhS to study,” Hamilton said. “We mounted and polished the tiny shard and used an infrared microscope to examine its composition. Spectral analysis identified a range of hydrated minerals, in particular amphibole, which points to intermediate temperatures and pressures and a prolonged period of aqueous alteration on a parent asteroid at least 400, and up to 1,100, miles in diameter.”
Amphiboles are rare in CC meteorites, having only been identified previously as a trace component in the Allende meteorite. “AhS is a serendipitous source of information about early Solar System materials that are not represented by CC meteorites in our collections,” Hamilton said.
Orbital spectroscopy of asteroids Ryugu and Bennu visited by Japan’s Hayabusa2 and NASA’s OSIRIS-REx spacecraft this year is consistent with aqueously altered CC meteorites and suggests that both asteroids differ from most known meteorites in terms of their hydration state and evidence for large-scale, low-temperature hydrothermal processes. These missions have collected samples from the surfaces of the asteroids for return to Earth.
“If the compositions of the Hayabusa2 and OSIRIS-REx samples differ from what we have in our collections of meteorites, it could mean that their physical properties cause them to fail to survive the processes of ejection, transit and entry through Earth’s atmosphere, at least in their original geologic context,” said Hamilton, who also serves on the OSIRIS-REx science team. “However, we think that there are more carbonaceous chondrite materials in the Solar System than are represented by our collections of meteorites.”
Contacts and sources:
Southwest Research Institute
Publication: Meteoritic evidence for a Ceres-sized water-rich carbonaceous chondrite parent asteroid.
V. E. Hamilton, C. A. Goodrich, A. H. Treiman, H. C. Connolly, M. E. Zolensky, M. H. Shaddad. Nature Astronomy, 2020; DOI: 10.1038/s41550-020-01274-z
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