Chemical evolution of OB associations

Details Chemical evolution of OB associations Chemical evolution of OB associations

Oct 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982nyasa.395..236s&link_type=abstract

(NASA, National Science Foundation, New York Academy of Sciences, et al., Symposium on the Orion Nebula to Honor Henry Draper, N

Other

11

B Stars, Chemical Evolution, Isotopic Enrichment, O Stars, Solar System, Stellar Evolution, Aluminum 26, Interstellar Matter, Palladium, Radioactive Age Determination, Supernovae

Scientific paper

It is determined that the existence of Al-26 and Pd-107 in meteorites in the early solar system indicates that our solar system probably formed inside an OB association that had been contaminated by the debris of at least one supernova. In addition to these radioactive tracers, the contamination of the material out of which the solar system formed would have significantly enriched the heavy element composition of the solar system relative to that of the average interstellar medium. It is found that the solar system would be enriched in those isotopes which are produced by the more massive stars, such as O-16, C-12, Ne-20, and some other r-process material. It is proposed that specific isotopic ratios and elemental ratios reflecting these differences would include the Ne-20/Ne-22 ratio, which would be higher in the solar system than in the interstellar medium and the cosmic rays, the C-12/C-13 ratio which would be higher in the solar system than in the interstellar medium, and the oxygen-to-carbon ratio, which would also be higher in the solar system than in the typical interstellar medium.

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