All Tables

Table 1: Basic parameters of selected WN+O SB2 binaries.
Table 2: Non-rotating WR+O progenitor models for $\beta =0.1$ . N is the number of the model, $M_{\rm 1,in}$ and $M_{\rm 2,in}$ are initial masses of the primary and the secondary, $p_{\rm in}$ is the initial orbital period and $q_{\rm in}$ is the initial mass ratio of the binary system. $t_{\rm A}$ is time when Case A mass transfer starts, $\Delta t_{\rm f}$ is the duration of the fast phase of Case A mass transfer, $\dot M_{\rm tr}^{\rm max}$ is the maximum mass transfer rate, $\Delta M_{\rm 1,f}$ and $\Delta M_{\rm 2,f}$ are mass loss of the primary and mass gain of the secondary (respectively) during fast Case A, $\Delta t_{\rm s}$ is the duration of slow Case A mass transfer, $\Delta M_{\rm 1,s}$ and $\Delta M_{\rm 2,s}$ are mass loss of the primary and mass gain of the secondary (respectively) during the slow Case A, $p_{\rm AB}$ is the orbital period at the onset of Case AB, $\Delta M_{\rm 1,AB}$ is the mass loss of the primary during Case AB (mass gain of the secondary is 1/10 of this, see Sect. 4), $M_{\rm WR,5}$ is the WR mass when the hydrogen surface abundance is $X_{\rm s}=0.05$ , the WR mass at $X_{\rm s}\le 0.01$ is given in brackets, $M_{\rm O}$ is the mass of the corresponding O star, q is the mass ratio $M_{\rm WR}/M_{\rm O}$ , 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 $^{\rm *}$ Hamann/3, $^{\rm **}$ 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, $M_{\rm 1,in}$ and $M_{\rm 2,in}$ are initial masses of the primary and the secondary, $p_{\rm in}$ is the initial orbital period and $q_{\rm in}$ is the initial mass ratio of the binary system. $t_{\rm A}$ is the time when Case A mass transfer starts, $\Delta t_{\rm f}$ is the duration of the the fast phase of Case A mass transfer, $\dot M_{\rm tr}^{\rm max}$ is the maximum mass transfer rate, $\Delta M_{\rm 1,f}$ and $\Delta M_{\rm 2,f}$ are mass loss of the primary and mass gain of the secondary (respectively) during the fast Case A, $\Delta t_{\rm s}$ is the duration of slow Case A mass transfer, $\Delta M_{\rm 1,s}$ and $\Delta M_{\rm 2,s}$ are mass loss of the primary and mass gain of the secondary (respectively) during the slow Case A, $p_{\rm AB}$ is the orbital period at the onset of Case AB, $\Delta M_{\rm 1,AB}$ is the mass loss of the primary during Case AB (mass gain of the secondary is 1/10 of this, see Sect. 4), $M_{\rm WR,5}$ is the WR mass when the hydrogen surface abundance is $X_{\rm s}=0.05$ , $M_{\rm O}$ is the mass of the corresponding O star, q is the mass ratio $M_{\rm WR}/M_{\rm O}$ , p is the orbital period of the WR+O system and $M_{\rm WR,1}$ is WR mass with $X_{\rm s}/le0.01$ . The models are computed with a stellar wind mass loss of Hamann/6 except : $^{\rm *}$ Hamann/3, $^{\rm **}$ 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. $M_{\rm 1,in},M_{\rm 2,in}$ are initial primary and secondary mass, $p_{\rm in}$ is the initial orbital period, $M_{\rm WR,5}$ , $M_{\rm WR,1}$ are WR masses at $X_{\rm s}=0.05$ and $X_{\rm s}\le 0.01$ respectively and p is the orbital period in the initial WR+O system where the hydrogen surface abundance of WR star is $X_{\rm s}=0.05$ . Systems are modelled with WR stellar wind mass loss H/6 except $^{\rm *}$ which are done with H/3, $^{\rm R}$ indicates rotating models.
Table 5: Mass loss from binary systems. N is number of the model corresponding to Table 3. $\bar \beta_{\rm fast}$ is the average accretion efficiency of the secondary during the fast phase of Case A mass transfer. $\bar \beta_{\rm slow}$ 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. ${\bar \beta_{\rm slow}}^{\rm wind}$ 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. $\bar \beta$ 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 ${\bar \beta_{\rm mtr}}^{\rm wind}$ taking also into account stellar wind mass loss of the primary.