All Figures

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{4030fig1.eps}\end{figure}$ Figure 1: Wolf-Rayet wind mass loss rates as a function of the stellar luminosity for a surface composition of X=0.15, Y=0.83, and Z=0.02. The mass loss rates by Hamann et al. (1995, HKW95) and Nugis & Lamers (2000, NL00) are given by the solid and dashed lines, respectively. The upper and lower dotted lines denote the HKW95 rates divided by a factor of 6 and 15 respectively, as assumed in this study. The filled circle and the open triangle are the mass loss rates given by Vink & de Koter (2005) for WN stars, with two different assumed values of $\beta$ , which determines the wind velocity law (see Vink & de Koter 2005 for the exact definition of $\beta$ ).
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{4030fig2.eps}\end{figure}$ Figure 2: Evolutionary tracks for models of Seq. 3 (dashed line) and Seq. 4 (solid line), in the HR diagram (cf. Table 1), from the zero age main sequence to core carbon exhaustion.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4030fig3.eps} \end{figure}$ Figure 3: Evolution of the internal structure of Seq. A4 from zero-age main sequence to the neon burning. Convective layers are hatched. Semi-convective layers are marked by dots (red dots in the electronic version). The gray shading gives nuclear energy generation rates in log scale, as indicated on the right side. The topmost solid line denotes the surface of the star.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4030fg4a.eps}\par\vspace*{2mm} \includegraphics[width=8.8cm,clip]{4030fg4b.eps} \end{figure}$ Figure 4: Upper panel: mass fraction of chemical elements after core carbon exhaustion in Seq. A3, as a function of the mass coordinate. lower panel: same as in the upper panel, but for model Seq. A4.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{4030fg5a.eps}\par\vspace*{2mm} \includegraphics[width=8.4cm,clip]{4030fg5b.eps}\end{figure}$ Figure 5: Mean specific angular momentum over the shells as a function of the mass coordinate at 4 different epochs in Seq. A3 ( upper panel) and Seq. A4 ( lower panel). Note that the equatorial specific angular momentum is larger by a factor of 1.5. The thin two-dotted-dashed line denotes the angular momentum of the last stable orbit around a non-rotating Schwardzschild black hole of mass equal to the mass coordinate. The thin long-dashed line gives the same but for a maximally rotating Kerr black hole. The thin dotted line denotes the specific angular momentum for the last stable orbit at the given mass of a black hole, assuming that all mass below forms a rotating black hole. Here, if the contained angular momentum is larger than that of a maximally rotating black hole, the black hole is assumed to rotate maximally.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{4030fig6.eps} \end{figure}$ Figure 6: Elapsed time from core helium exhaustion to the core carbon exhaustion, for Seqs. A1 (20 $\ensuremath {{M}_\odot }$ ), A2 (30 $\ensuremath {{M}_\odot }$ ), A4 (40 $\ensuremath {{M}_\odot }$ ), A5 (50 $\ensuremath {{M}_\odot }$ ), and A6 (60 $\ensuremath {{M}_\odot }$ ).
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{4030fg7a.eps}\par\vspace*{2mm} \includegraphics[width=7.6cm,clip]{4030fg7b.eps}\end{figure}$ Figure 7: Specific angular momentum as a function of the mass coordinate, in the last models of Seqs. C1 ( upper panel) and C2 ( lower panel) (after core carbon exhaustion in Seq. C1 and near the core carbon exhaustion ( $X_{\rm C} = 10^{-4}$ ) in Seq. C2). The thick solid line denotes the mean specific angular momentum over the shells, as function of the mass coordinate. The thick dashed line gives the equatorial specific angular momentum. The thin two-dotted-dashed line denotes the angular momentum of the last stable orbit around a non-rotating Schwardzschild black hole of mass equal to the mass coordinate. The thin long-dashed line gives the same but for a maximally rotating Kerr black hole. The thin dotted line denotes the specific angular momentum of the last stable orbit at the given mass of a black hole, assuming that all mass below forms a rotating black hole. Here, if the contained angular momentum is larger than that of a maximally rotating black hole, the black hole is assumed to rotate maximally.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{4030fig2.eps}\end{figure}$	Figure 2: Evolutionary tracks for models of Seq. 3 (dashed line) and Seq. 4 (solid line), in the HR diagram (cf. Table 1), from the zero age main sequence to core carbon exhaustion.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4030fig3.eps} \end{figure}$	Figure 3: Evolution of the internal structure of Seq. A4 from zero-age main sequence to the neon burning. Convective layers are hatched. Semi-convective layers are marked by dots (red dots in the electronic version). The gray shading gives nuclear energy generation rates in log scale, as indicated on the right side. The topmost solid line denotes the surface of the star.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{4030fg4a.eps}\par\vspace*{2mm} \includegraphics[width=8.8cm,clip]{4030fg4b.eps} \end{figure}$	Figure 4: Upper panel: mass fraction of chemical elements after core carbon exhaustion in Seq. A3, as a function of the mass coordinate. lower panel: same as in the upper panel, but for model Seq. A4.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{4030fig6.eps} \end{figure}$	Figure 6: Elapsed time from core helium exhaustion to the core carbon exhaustion, for Seqs. A1 (20 $\ensuremath {{M}_\odot }$ ), A2 (30 $\ensuremath {{M}_\odot }$ ), A4 (40 $\ensuremath {{M}_\odot }$ ), A5 (50 $\ensuremath {{M}_\odot }$ ), and A6 (60 $\ensuremath {{M}_\odot }$ ).
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