Origin of Ca-Al-rich inclusions. II - Sputtering and collisions in the three-ph8se interstellar medium

Details Origin of Ca-Al-rich inclusions. II - Sputtering and collisions in the three-ph8se interstellar medium Origin of Ca-Al-rich inclusions. II - Sputtering and collisions in the three-ph8se interstellar medium

Dec 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981apj...251..374c&link_type=abstract

Astrophysical Journal, Part 1, vol. 251, Dec. 1, 1981, p. 374-386. Research supported by the Max-Planck-Institut für Kernphysik

Other

16

Aluminum, Calcium, Interstellar Matter, Meteoritic Composition, Planetary Evolution, Solar System, Cosmochemistry, Inclusions, Nebulae, Nuclear Fusion, Supernova Remnants

Scientific paper

The theory put forward by Clayton (1977) for the formation of the Ca-Al-rich inclusions within C3 meteorites is extended to an evolutionary history in a three-phase interstellar medium. Widespread supersonic turbulence in the hot interstellar medium is maintained by supernova shock waves, giving rise to heavy sputtering of the refractory dust. Subsequent reaccumulation with varying dust/gas ratios or varying particle sizes produces isotopically fractionated Ca-Al-rich accumulates. It is thought that the Ca-Al-rich inclusions themselves are formed by the following sequence in the solar system: (1) cold accumulation of larger-than-average Ca-Al-rich particles containing supernova condensate cores into macroscopic (approximately 1 cm) Ca-Al-rich agglomerates, probably by sedimentation; and (2) fusion of the supernova condensates into macroscopic minerals by exothermic chemical reactions that begin when the accumulate has been warmed, thereby releasing energy from the unequilibrated forms accumulated from the interstellar medium.

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