The stellar upper mass limit in an OB association and implications for cosmic rays and cosmic abundances

Details The stellar upper mass limit in an OB association and implications for cosmic rays and cosmic abundances The stellar upper mass limit in an OB association and implications for cosmic rays and cosmic abundances

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986icr..conf....9b&link_type=abstract

In its Contributions to the 18th International Cosmic Ray Conference p 9-12 (SEE N87-13389 04-93)

Physics

Cosmic Rays, Nebulae, Protostars, Solar System, Star Formation, Sun, Aluminum 26, Interstellar Matter, Nuclear Fusion, Palladium Isotopes, Stellar Winds, Supernovae

Scientific paper

Some implications are considered of the possibility that the collapse of the solar nebula was induced by the supernova of an extremely massive star or, at least, such a star was in the vicinity of the protosolar nebula prior to its collapse to form the solar system. A very large star in the vicinity of the protosolar nebula can contribute to the protosolar nebula in several ways which differ from a smaller (but still large) star: (1) the high mass-loss rate of a very large star implies the dispersion into the nearby interstellar medium of many solar masses of freshly synthesized material (a substantial dilution can occur before its contribution is masked); (2) a significant amount of Al-26 is synthesized and dispersed well before the subsequent supernova; (3) energy is available in the stellar wind for accelerating cosmic rays in sufficient quantities to heavily irradiate nearby material; (4) the absence of freshly synthesized Pu-244 (no resetting of the plutonium clock) can be understood in a natural way; and (5) a significant amount of Pd-107 can be dispersed into the interstellar medium during a WC stage.

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