Other
Scientific paper
Oct 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004esasp.552...99h&link_type=abstract
Proceedings of the 5th INTEGRAL Workshop on the INTEGRAL Universe (ESA SP-552). 16-20 February 2004, Munich, Germany. Scientific
Other
Scientific paper
Recent analyses of the 1.809 MeV emission from the decay of long-lived radioactive 26 Al the in the nearest Wolfe-Rayet (WR) star and nearby OB associations are not consistent with standard models of the origin of Galactic 26 Al and set challenging new constraints on the possible sources. The winds of massive WR stars have recently been considered the most likely source of 26 Al, but the expected 26 Al yield from the nearest WR star exceeds by as much as a factor of 3, that set by the 2-σ upper limit on the 1.809 MeV emission. Yet the expected 26 Al yields from WR stars in three of the largest nearby (<2 kpc) OB associations are only about 1/3 of that required to account for their 1.809 MeV emission, while at the same time, no detectable 1.809 emission has been reported from the six other large, nearby OB associations. We have proposed that the solution to these problems may lie in 26 Al from a previously ignored source: explosive nucleosynthesis in the core collapse SNIb/c supernovae of WR stars that have lost most of their mass to close binary companions. Recent nucleosynthetic calculations of SNIb/c suggest that their 26 Al yields depend very strongly on the final, pre-supernova mass of the WR star, and that those with final masses around 6 to 8 M are expected to produce as much as 10-2 M of 26 Al per supernova. Such binary SNIb/c make up only a small fraction of the current SNIb/c and only about 1% of all Galactic core collapse supernovae. But they appear to be such prolific sources that the bulk of the present 26 Al in the Galaxy may come from just a few hundred close binary SNIb/c and the intense 1.809 MeV emission from nearby OB associations may come from just one or two such supernova. The INTEGRAL survey of Galactic sources of 26 Al can provide crucial tests of this possibility.
Higdon James C.
Lingenfelter Richard E.
Rothschild Richard E.
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