Astronomy and Astrophysics – Astronomy
Scientific paper
Dec 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995mnras.277.1080l&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 277, Issue 3, pp. 1080-1086.
Astronomy and Astrophysics
Astronomy
25
Stars: Abundances, Binaries: General, Blue Stragglers, Stars: Rotation, Open Clusters And Associations: General
Scientific paper
O- and B-type runaway stars can be produced either by supernova explosions in massive close binary systems (i.e., supernova ejection) or via strong dynamical interactions in young star clusters (i.e., dynamical or cluster ejection). Blaauw has suggested that the majority of the OB runaways are a result of supernova ejection, because the majority appear to have the rapid rotations and higher-than-average helium abundances that are expected for stars that have been on the receiving end of mass transfer in massive close binary systems. Physical stellar collisions can occur during the binary-binary interactions that produce dynamically ejected runaway stars, however, and the resulting merged stars have rapid rotations and higher-than-average helium abundances. Binary-binary scattering experiments reveal that some of the merged stars attain speeds large enough to classify them as runaways. Consequently, the predictions of the supernova and dynamical ejection hypotheses are not as distinct as had been previously believed. A very careful observational study of the rotational rates and helium abundances of an unbiased sample of OB runaway stars will be required to discriminate between the two hypotheses for their origin.
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