All Figures

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fig1.eps} \end{figure}$ Figure 1: Masses of both components of post-Case A mass transfer WR+O binary systems resulting from our simple approach, for initial primary masses in the range 25...100 $~{M}_{\odot}$ and an initial period of $p_{\rm in}=3$ days, for four different assumed accretion efficiencies $\beta$ ( a)- d)). The solid line represents a mass ratio of $q=M_{\rm WR}/M_{\rm O}=0.5$ . For an increasing $\beta$ , the O stars in WR+O systems become more massive and the WR/O-mass ratio decreases.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fig2.eps} \end{figure}$ Figure 2: Masses of both components of post-Case A mass transfer WR+O binary systems resulting from our simple approach, for initial primary masses in the range 25...100 $~{M}_{\odot}$ and for early ( $p_{\rm in}=3$ days) Case A and late Case A respective Case B evolution. The assumed accretion efficiency is $\beta =0...1$ . The solid line represents a mass ratio of $q=M_{\rm WR}/M_{\rm O}=0.5$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2368fig3.eps} \end{figure}$ Figure 3: HR diagram of the initial system $M_{\rm 1,in}=56~{M}_{\odot}$ , $M_{\rm 2,in}=33~{M}_{\odot}$ , $p_{\rm in}=6$ days. Both stars are core hydrogen burning (dashed line) until Case A mass transfer starts (solid line). The primary is losing mass and its luminosity and effective temperature decrease. At the same time the secondary is accreting matter and expanding, becoming more luminous and cooler. After Case A mass transfer is finished, the primary is losing mass by stellar wind and contracting at the end of core hydrogen burning (dotted line). After this the primary starts with shell hydrogen burning and expands (dash-dotted line).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2368fig4.eps} \end{figure}$ Figure 4: The evolution of the internal structure of the 56 $~{M}_{\odot}$ primary during the core hydrogen burning. Convection is indicated with diagonal hatching and semiconvection with crossed hatching. The hatched area at the bottom indicates nuclear burning. The topmost solid line corresponds to the surface of the star.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fig5.eps} \end{figure}$ Figure 5: The evolution of the internal structure of the 33 $~{M}_{\odot}$ secondary during core hydrogen burning of the primary. Convection is indicated with diagonal hatching, semiconvection with crossed hatching and thermohaline mixing with straight crossed hatching. The hatched area at the bottom indicates nuclear burning. The topmost solid line corresponds to the surface of the star.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2368fig6.eps} \end{figure}$ Figure 6: Upper plot: mass transfer rate during Case A mass transfer in the binary system with $M_{\rm 1,in}=56~{M}_{\odot}$ , $M_{\rm 2,in}=33~{M}_{\odot}$ , $p_{\rm in}=6$ days. Lower plot: the hydrogen surface abundance of the primary (solid line) is decreasing during mass transfer and further due to stellar wind mass loss. The secondary (dashed line) recovered its original surface hydrogen abundance through thermohaline mixing. The primary starts losing mass with WR stellar wind mass loss when its hydrogen surface abundance falls beneath $X_{\rm s}=0.4$ , represented by the dotted line.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fig7.eps} \end{figure}$ Figure 7: Surface abundance of carbon (solid line), nitrogen (dotted line) and oxygen (dashed line) of the primary ( upper plot) and the secondary ( lower plot) in the system with $M_{\rm 1,in}=56~{M}_{\odot}$ , $M_{\rm 2,in}=33~{M}_{\odot}$ , $p_{\rm in}=6$ days.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fig8.eps} \end{figure}$ Figure 8: Initial WR mass as a function of initial (progenitor) mass. Large and small symbols indicate WR stars with hydrogen surface abundance of $X_{\rm s}=0.05$ and $X_{\rm s}\le 0.01$ , respectively. Systems with an initial orbital period of $p_{\rm in}=3$ days and a mass ratio of $q\sim 1.7$ are indicated with star symbols, systems with an initial period of 6 days and $q\sim 1.7$ with diamond symbols, systems with an initial primary 41 $~{M}_{\odot}$ and initial period of 3 days with triangle symbols. The dashed line represents a linear fit for systems with an initial period of 3 days and with $X_{\rm s}=0.05$ , and the dotted line represents linear fit for systems with an initial period of 3 days and $X_{\rm s}\le 0.01$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fig9.eps} \end{figure}$ Figure 9: Mass transfer rate ( upper plot) and orbital period ( lower plot) during Case A mass transfer as a function of the change of the primary mass for systems with the initial primary $M_{\rm 1,in}=41~{M}_{\odot}$ , initial orbital period $p_{\rm in}=3$ days and four different initial mass ratios: 2.00 (dotted line), 1.71 (solid line), 1.52 (dashed line) and 1.37 (dash-dotted line). (Table 2: N 3, 4, 6, 7)
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fg10.eps} \end{figure}$ Figure 10: Mass transfer rate during Case A mass transfer for systems 41 $~{M}_{\odot}$ +24 $~{M}_{\odot}$ ( upper plot) and 56 $~{M}_{\odot}$ +33 $~{M}_{\odot}$ ( lower plot) and an initial orbital period of $p_{\rm in}=3$ days (solid line) and $p_{\rm in}=6$ days (dashed line). Case A mass transfer starts later in initially wider binary systems, the primary has more time to increase mass of its core and the initial WR star is more massive (Table 2: N 4, 5, 9, 10).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2368fg11.eps} \end{figure}$ Figure 11: Primary mass ( first plot), mass transfer rate ( second plot) and stellar wind mass loss rate from the primary (third plot) until the onset of Case AB mass transfer for the system $M_{\rm 1,in}=56~{M}_{\odot}$ , $M_{\rm 2,in}=33~{M}_{\odot}$ , $p_{\rm in}=6$ days and three different stellar wind mass loss rates (from $X_{\rm s}\le 0.4$ ): 1/6 (solid line), 1/3 (dotted line) and 1/2 (dashed line) of mass loss rate proposed by Hamann et al. (1995) (Table 2: N 10, 11, 12).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2368fg12.eps} \end{figure}$ Figure 12: HR diagram of the initial system $M_{\rm 1,in}=56~{M}_{\odot}$ , $M_{\rm 2,in}=33~{M}_{\odot}$ , $p_{\rm in}=6$ days with rotation. Both stars are core hydrogen burning (dashed line) until Case A mass transfer starts (solid line). The primary is losing mass and its luminosity decreases. At the same time the secondary is accreting matter and expanding, becoming more luminous. After Case A mass transfer is finished, the primary is losing mass by stellar wind and contracting at the end of core hydrogen burning (dotted line). After this the primary starts shell hydrogen burning and expands (dash-dotted line).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fg13.eps} \end{figure}$ Figure 13: The evolution of the internal structure of the rotating 56 $~{M}_{\odot}$ primary during core hydrogen burning. Convection is indicated with diagonal hatching and semiconvection with crossed hatching. The hatched area at the bottom indicates nuclear burning. Gray shaded areas represent regions with rotationally induced mixing (intensity is indicated with different shades, the darker the colour, the stronger rotational mixing). The topmost solid line corresponds to the surface of the star.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fg14.eps} \end{figure}$ Figure 14: The evolution of the internal structure of the rotating 33 $~{M}_{\odot}$ secondary during core hydrogen burning of the primary. Convection is indicated with diagonal hatching, semiconvection with crossed hatching and thermohaline mixing with straight crossed hatching. The hatched area at the bottom indicates nuclear burning. Gray shaded areas represent regions with rotationally induced mixing (intensity is indicated with different shades, the darker the colour, the stronger rotational mixing). The topmost solid line corresponds to the surface of the star.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2368fg15.eps} \end{figure}$ Figure 15: Upper plot: the mass transfer rate during Case A mass transfer in the binary systems with $M_{\rm 1,in}=56~{M}_{\odot}$ , $M_{\rm 2,in}=33~{M}_{\odot}$ , $p_{\rm in}=6$ days with (solid line) and without rotation (dotted line). Lower plot: orbital period evolution in rotating and non-rotating system.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fg16.eps} \end{figure}$ Figure 16: The hydrogen surface abundance (solid line) in the primary in system with $M_{\rm 1,in}=56~{M}_{\odot}$ , $M_{\rm 2,in}=33~{M}_{\odot}$ , $p_{\rm in}=6$ days is decreasing during mass transfer and further due to stellar wind mass loss. The secondary (dashed line) decreases its hydrogen surface abundance due to mass transfer. The dotted line indicates a hydrogen abundance of 0.4, where the primary starts losing mass with a WR stellar wind.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fg17.eps} \end{figure}$ Figure 17: Surface abundance of carbon (solid line), nitrogen (dotted line) and oxygen (dashed line) in the primary ( upper plot) and the secondary ( lower plot), in the system with $M_{\rm 1,in}=56~{M}_{\odot}$ , $M_{\rm 2,in}=33~{M}_{\odot}$ , $p_{\rm in}=6$ days. The secondary abundances are changed due to mass transfer of matter from the primary, thermohaline mixing and rotational mixing.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fg18.eps} \end{figure}$ Figure 18: The orbital angular momentum ( upper plot) of the non-rotating (dotted line) and the rotating (solid line) binary systems with $M_{\rm 1,in}=56~{M}_{\odot}$ , $M_{\rm 2,in}=33~{M}_{\odot}$ , $p_{\rm in}=6$ days, decreases rapidly due to mass loss from the system during fast Case A mass transfer and then further due to stellar wind mass loss. Spin period ( lower plot) of the primary (dashed line) and the secondary (dash-dotted line) in the above mentioned rotating binary system.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fg19.eps} \end{figure}$ Figure 19: Effective temperature (plot a)), stellar radius (plot b)), stellar wind mass loss rate (plot c)) and rotational velocity (plot d)) of the primary star in the non-rotating (dotted line) and rotating (solid line) binary system with $M_{\rm 1,in}=56~{M}_{\odot}$ , $M_{\rm 2,in}=33~{M}_{\odot}$ , $p_{\rm in}=6$ days.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fg20.eps} \end{figure}$ Figure 20: Effective temperature (plot a)), stellar radius (plot b)), stellar wind mass loss rate (plot c)) and rotational velocity (plot d)) of the secondary star in the non-rotating (dotted line) and rotating (solid line) binary system with $M_{\rm 1,in}=56~{M}_{\odot}$ , $M_{\rm 2,in}=33~{M}_{\odot}$ , $p_{\rm in}=6$ days.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fg21.eps} \end{figure}$ Figure 21: Upper plot: mass transfer (solid line) and accretion rate (dotted line) of the rotating initial system 56 $~{M}_{\odot}+33~{M}_{\odot}$ , p=6 days. Dashed line represent mass transfer rate in the corresponding non-rotating binary. Lower plot: accretion efficiency of the secondary taking into account matter lost by the primary only due to mass transfer.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2368fig4.eps} \end{figure}$	Figure 4: The evolution of the internal structure of the 56 $~{M}_{\odot}$ primary during the core hydrogen burning. Convection is indicated with diagonal hatching and semiconvection with crossed hatching. The hatched area at the bottom indicates nuclear burning. The topmost solid line corresponds to the surface of the star.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fig5.eps} \end{figure}$	Figure 5: The evolution of the internal structure of the 33 $~{M}_{\odot}$ secondary during core hydrogen burning of the primary. Convection is indicated with diagonal hatching, semiconvection with crossed hatching and thermohaline mixing with straight crossed hatching. The hatched area at the bottom indicates nuclear burning. The topmost solid line corresponds to the surface of the star.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fig7.eps} \end{figure}$	Figure 7: Surface abundance of carbon (solid line), nitrogen (dotted line) and oxygen (dashed line) of the primary ( upper plot) and the secondary ( lower plot) in the system with $M_{\rm 1,in}=56~{M}_{\odot}$ , $M_{\rm 2,in}=33~{M}_{\odot}$ , $p_{\rm in}=6$ days.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2368fg15.eps} \end{figure}$	Figure 15: Upper plot: the mass transfer rate during Case A mass transfer in the binary systems with $M_{\rm 1,in}=56~{M}_{\odot}$ , $M_{\rm 2,in}=33~{M}_{\odot}$ , $p_{\rm in}=6$ days with (solid line) and without rotation (dotted line). Lower plot: orbital period evolution in rotating and non-rotating system.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fg19.eps} \end{figure}$	Figure 19: Effective temperature (plot a)), stellar radius (plot b)), stellar wind mass loss rate (plot c)) and rotational velocity (plot d)) of the primary star in the non-rotating (dotted line) and rotating (solid line) binary system with $M_{\rm 1,in}=56~{M}_{\odot}$ , $M_{\rm 2,in}=33~{M}_{\odot}$ , $p_{\rm in}=6$ days.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fg20.eps} \end{figure}$	Figure 20: Effective temperature (plot a)), stellar radius (plot b)), stellar wind mass loss rate (plot c)) and rotational velocity (plot d)) of the secondary star in the non-rotating (dotted line) and rotating (solid line) binary system with $M_{\rm 1,in}=56~{M}_{\odot}$ , $M_{\rm 2,in}=33~{M}_{\odot}$ , $p_{\rm in}=6$ days.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2368fg21.eps} \end{figure}$	Figure 21: Upper plot: mass transfer (solid line) and accretion rate (dotted line) of the rotating initial system 56 $~{M}_{\odot}+33~{M}_{\odot}$ , p=6 days. Dashed line represent mass transfer rate in the corresponding non-rotating binary. Lower plot: accretion efficiency of the secondary taking into account matter lost by the primary only due to mass transfer.
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