Table 4:
Comparison of resulting WR masses and orbital periods from
non-rotating and rotating binary systems with the same initial parameters.
are
initial primary and secondary mass,
is the initial orbital period,
,
are WR masses at
and
respectively
and p is the orbital period in the initial WR+O system where the hydrogen surface abundance of WR star is
.
Systems are modelled with WR stellar wind mass loss H/6 except
which are done with H/3,
indicates rotating models.