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Astron. Astrophys. 318, 812-818 (1997)

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4. Conclusions

A detailed population synthesis model including the evolutionary effects of massive close binaries with periods ranging from 1 day to 10 years and the effect of an asymmetric SN explosion of the primary and of the secondary, reveals the following general conclusions:

[FORMULA] At least 50% of the observed O-type runaways are formed through the binary scenario and only 12-17% of the O-type runaways have a compact companion.

[FORMULA] Only 1% - 3% of all WR stars may hide a compact companion.

[FORMULA] We expect a binary pulsar formation rate of the order of 10-5 /year, corresponding to the formation rate which is based on the observed number of binary pulsars and their expected lifetime.

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© European Southern Observatory (ESO) 1997

Online publication: July 3, 1998
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