- Table 1: Basic parameters of selected WN+O SB2 binaries.
- Table 2:
Non-rotating WR+O progenitor models for .
*N*is the number of the model, and are initial masses of the primary and the secondary, is the initial orbital period and is the initial mass ratio of the binary system. is time when Case A mass transfer starts, is the duration of the fast phase of Case A mass transfer, is the maximum mass transfer rate, and are mass loss of the primary and mass gain of the secondary (respectively) during fast Case A, is the duration of slow Case A mass transfer, and are mass loss of the primary and mass gain of the secondary (respectively) during the slow Case A, is the orbital period at the onset of Case AB, is the mass loss of the primary during Case AB (mass gain of the secondary is 1/10 of this, see Sect. 4), is the WR mass when the hydrogen surface abundance is , the WR mass at is given in brackets, is the mass of the corresponding O star,*q*is the mass ratio , and*p*is the orbital period of the WR+O system. The models are computed with a stellar wind mass loss of Hamann/6, except Hamann/3, Hamann/2.

*c*indicates a contact phase that occurs for low masses due to a mass ratio too far from unity, for high masses due to the secondary expansion during slow phase of Case A. - Table 3:
Rotating WR+O progenitor models.
*N*is the number of the model, and are initial masses of the primary and the secondary, is the initial orbital period and is the initial mass ratio of the binary system. is the time when Case A mass transfer starts, is the duration of the the fast phase of Case A mass transfer, is the maximum mass transfer rate, and are mass loss of the primary and mass gain of the secondary (respectively) during the fast Case A, is the duration of slow Case A mass transfer, and are mass loss of the primary and mass gain of the secondary (respectively) during the slow Case A, is the orbital period at the onset of Case AB, is the mass loss of the primary during Case AB (mass gain of the secondary is 1/10 of this, see Sect. 4), is the WR mass when the hydrogen surface abundance is , is the mass of the corresponding O star,*q*is the mass ratio ,*p*is the orbital period of the WR+O system and is WR mass with . The models are computed with a stellar wind mass loss of Hamann/6 except : Hamann/3, Hamann/2.

*c*indicates a contact phase. - 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. - Table 5:
Mass loss from binary systems.
*N*is number of the model corresponding to Table 3. is the average accretion efficiency of the secondary during the fast phase of Case A mass transfer. is the accretion efficiency of the secondary during the slow phase of Case A mass transfer taking into account matter lost by the primary only due to the mass transfer. is the average accretion efficiency of the secondary during the slow phase of Case A mass transfer taking into account matter lost by the primary due to the mass transfer and stellar wind. is the average accretion efficiency of the secondary during the progenitor evolution of WR+O binary system taking into account matter lost by the primary only due to the mass transfer and taking also into account stellar wind mass loss of the primary.