Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2545fig1.eps} \end{figure}$ Figure 1: Specific angular momentum profiles of a 20 $~{M}_{\odot}$ single star on the hydrogen ZAMS (three dots-dashed line), when helium ignites in the core, (dot-dashed line), when the central helium abundance is 67% (dashed-line), in the moment of core helium exhaustion (dotted line) and at core carbon exhaustion (solid line).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fig2.eps} \end{figure}$ Figure 2: Logarithm of the integrated angular momentum, $J(m)=\int_{0}^{M}j(m^{\prime}){\rm d}m^{\prime}$ divided by m^5/3, as a function of the mass coordinate, m, for a 20 $~{M}_{\odot}$ star for the same evolutionary stages as shown in Fig. 1. The thin lines give a logarithmic scale of levels of constant J labeled with $\log(J/\rm (erg~s))$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2545fig3.eps} \end{figure}$ Figure 3: Specific angular momentum profiles of a 42 $~{M}_{\odot}$ single star on the hydrogen ZAMS (dot-dashed line), when helium ignites in the center (dotted line), and when the central helium abundance is 67% (solid line).
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2545fig4.eps} \end{figure}$ Figure 4: Logarithm of the integrated angular momentum $J(m)=\int_{0}^{M}j(m^{\prime}){\rm d}m^{\prime}$ divided by m^5/3, as a function of the mass coordinate m for a 42 $~{M}_{\odot}$ star for the same evolutionary stages as shown in Fig. 3. The thin lines give a logarithmic scale of levels of constant J labeled with $\log(J/\rm (erg~s))$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2545fig5.eps} \end{figure}$ Figure 5: Evolutionary track of the primary in HR diagram. Solid line: core hydrogen burning phase before and after Case A mass transfer. Dotted line: Case A mass transfer. Dashed line: connection between last calculated model at the onset of Case AB and first calculated model when the primary is a hydrogen-free WR star. Dash-dotted line: core helium burning phase. Dot-dashed line: core carbon burning phase.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2545fig6.eps} \end{figure}$ Figure 6: Evolutionary track of the secondary in the HR diagram. Solid line: core hydrogen burning phase before and after Case A and Case AB mass transfer. Dotted line: Case A mass transfer. Dash-dotted line: core helium burning phase.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2545fig7.eps} \end{figure}$ Figure 7: Evolution of the internal structure of a rotating 33 $~{M}_{\odot}$ secondary from the ZAMS until red supergiant phase $Y_{\rm c}=0.67$ . 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

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2545fig8.eps} \end{figure}$ Figure 8: Evolution of the internal structure of a rotating 33 $~{M}_{\odot}$ secondary from SN explosion of the primary and disruption of the system. See Fig. 7 for an explanation of the different hatching types.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2545fig9.eps} \end{figure}$ Figure 9: Surface rotational velocity of the secondary star. Matter transfered from the primary with high mass transfer rate $\sim$ 10^-3-10 $^{-4} ~{M}_{\odot} ~\rm yr^{-1}$ during the fast phase of Case A and Case AB spins up the surface layers of the secondary up to 500-700 $\rm ~km~s^{-1}$ . During the slow phase of Case A mass transfer rate is lower ( $\sim$ 10 $^{-6}~{M}_{\odot} \rm ~yr^{-1}$ ) and surface rotational velocity increases up to $\sim$ 200 $\rm ~km~s^{-1}$ . After Case AB mass transfer the secondary synchronizes with the orbital motion in the WR+O binary system. After the SN explosion of the primary, the secondary star evolves into a red supergiant with slowly rotating envelope of $\sim$ 0.02 km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2545fg10.eps} \end{figure}$ Figure 10: Rotational velocity profiles of the secondary star on the hydrogen ZAMS (solid line), after the fast (dotted line) and the slow (short dashed line) phase of Case A mass transfer, after Case AB mass transfer (dash-dotted line), when helium ignites in the core (three dots-dashed line) and when the central helium abundance is 67% (long dashed-line).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fg11.eps} \end{figure}$ Figure 11: Specific angular momentum profiles of the secondary star on the hydrogen ZAMS (long dashed line), after fast (dotted line) and slow (short dashed line) Case A mass transfer, after Case AB mass transfer (dash-dotted line), when helium ignites in the core (three dots-dashed line) and when the central helium abundance is 67% (solid line).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fg12.eps} \end{figure}$ Figure 12: Logarithm of the integrated angular momentum J(m)= $\int_{0}^{M}j(m^{\prime}){\rm d}m^{\prime}$ divided by m^5/3, as a function of the mass coordinate m for a 33 $~{M}_{\odot}$ secondary star for the same evolutionary stages as shown in Fig. 11. The thin lines give a logarithmic scale of levels of constant J labeled with $\log(J/\rm (erg~s))$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm]{2545fg13.eps} \end{figure}$ Figure 13: Specific angular momentum profiles of the secondary star on the hydrogen ZAMS (solid line) and when helium ignites in the core ( $T_{\rm c}=1.4\times 10^8 \rm ~K$ ), assuming the accretion of 0.25 $~{M}_{\odot}$ (dotted line) 1.4 $~{M}_{\odot}$ (dashed line) or 5 $~{M}_{\odot}$ (dot-dashed line) during Case AB mass transfer.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fg14.eps} \end{figure}$ Figure 14: Specific angular momentum profiles of the 42 $~{M}_{\odot}$ single star with magnetic fields on the hydrogen ZAMS (dot-dashed line), when 50% of hydrogen is left in the center (dotted line), when hydrogen is exhausted in the core (dashed line) and when central helium burning starts (solid line).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fg15.eps} \end{figure}$ Figure 15: Spin period profiles of the 42 $~{M}_{\odot}$ single star on the ZAMS (solid line), when 50% hydrogen is left in the center (dotted line), when hydrogen is exhausted in the core (dashed line), and when central helium burning starts (dot-dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fg16.eps} \end{figure}$ Figure 16: Stellar wind mass loss of the magnetic (dotted line) and non-magnetic (solid line) 42 $~{M}_{\odot}$ star. The star with magnetic fields loses more mass because magnetic torques transport angular momentum, which spins-up the surface layers and enhances mass loss.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fg17.eps} \end{figure}$ Figure 17: Effective viscosities due to magnetic torques (solid line) and due to rotational instabilities (dotted line) for a rotating 42 $~{M}_{\odot}$ star at a central hydrogen abundance of 50% and at core hydrogen exhaustion.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fg18.eps} \end{figure}$ Figure 18: Evolution of the internal structure of a rotating 33 $~{M}_{\odot}$ secondary star with magnetic field from the ZAMS until red supergiant phase $Y_{\rm c}=0.92$ . See Fig. 7 for an explanation of the different hatching types.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fg19.eps} \end{figure}$ Figure 19: Evolution of the internal structure of a rotating 33 $~{M}_{\odot}$ secondary star with magnetic field from after the SN explosion of the primary and disruption of the system. See Fig. 7 for an explanation of the different hatching types.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fg20.eps} \end{figure}$ Figure 20: Specific angular momentum profiles of the secondary star with magnetic fields on the hydrogen ZAMS (long dashed line), after fast (dotted line) and slow (short dashed line) Case A mass transfer, when all hydrogen is exhausted in the center (dot-dashed line), when helium ignites (three dots-dashed line) and and when the central helium abundance is 92% (solid line).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2545fg21.eps} \end{figure}$ Figure 21: Evolution of the internal structure of a rotating 33 $~{M}_{\odot}$ secondary star until helium ignition in the core. The star accretes 2 $~{M}_{\odot}$ when the central helium abundance is 95%. See Fig. 7 for an explanation of the different hatching types.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2545fg22.eps} \end{figure}$ Figure 22: Evolution of the internal structure of a rotating 33 $~{M}_{\odot}$ secondary star with magnetic field until helium ignition in the core. The star accretes 2 $~{M}_{\odot}$ when the central helium abundance is 95%. See Fig. 7 for an explanation of the different hatching types.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2545fg23.eps} \end{figure}$ Figure 23: Specific angular momentum profiles of a 33 $~{M}_{\odot}$ non-magnetic star on the ZAMS (long dashed line), when $Y_{\rm c}=95$ % (dotted line), at the end of the accretion (dashed line), 10 $^4\rm ~yr$ after the accretion (dot-dashed line), when hydrogen is exhausted in the core (three dot-dashed line) and when helium ignites in the core (solid line).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2545fg24.eps} \end{figure}$ Figure 24: Specific angular momentum profiles of a 33 $~{M}_{\odot}$ magnetic star on the ZAMS (long dashed line), when $Y_{\rm c}=95$ % (dotted line), at the end of the accretion (dashed line), 10 $^4\rm ~yr$ after the accretion (dot-dashed line), when hydrogen is exhausted in the core (three dot-dashed line) and when helium ignites in the core (solid line).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2545fig1.eps} \end{figure}$	Figure 1: Specific angular momentum profiles of a 20 $~{M}_{\odot}$ single star on the hydrogen ZAMS (three dots-dashed line), when helium ignites in the core, (dot-dashed line), when the central helium abundance is 67% (dashed-line), in the moment of core helium exhaustion (dotted line) and at core carbon exhaustion (solid line).
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fig2.eps} \end{figure}$	Figure 2: Logarithm of the integrated angular momentum, $J(m)=\int_{0}^{M}j(m^{\prime}){\rm d}m^{\prime}$ divided by m^5/3, as a function of the mass coordinate, m, for a 20 $~{M}_{\odot}$ star for the same evolutionary stages as shown in Fig. 1. The thin lines give a logarithmic scale of levels of constant J labeled with $\log(J/\rm (erg~s))$ .
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2545fig3.eps} \end{figure}$	Figure 3: Specific angular momentum profiles of a 42 $~{M}_{\odot}$ single star on the hydrogen ZAMS (dot-dashed line), when helium ignites in the center (dotted line), and when the central helium abundance is 67% (solid line).
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2545fig4.eps} \end{figure}$	Figure 4: Logarithm of the integrated angular momentum $J(m)=\int_{0}^{M}j(m^{\prime}){\rm d}m^{\prime}$ divided by m^5/3, as a function of the mass coordinate m for a 42 $~{M}_{\odot}$ star for the same evolutionary stages as shown in Fig. 3. The thin lines give a logarithmic scale of levels of constant J labeled with $\log(J/\rm (erg~s))$ .
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2545fig6.eps} \end{figure}$	Figure 6: Evolutionary track of the secondary in the HR diagram. Solid line: core hydrogen burning phase before and after Case A and Case AB mass transfer. Dotted line: Case A mass transfer. Dash-dotted line: core helium burning phase.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2545fig8.eps} \end{figure}$	Figure 8: Evolution of the internal structure of a rotating 33 $~{M}_{\odot}$ secondary from SN explosion of the primary and disruption of the system. See Fig. 7 for an explanation of the different hatching types.
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$\begin{figure} \par\includegraphics[width=8.5cm,clip]{2545fg10.eps} \end{figure}$	Figure 10: Rotational velocity profiles of the secondary star on the hydrogen ZAMS (solid line), after the fast (dotted line) and the slow (short dashed line) phase of Case A mass transfer, after Case AB mass transfer (dash-dotted line), when helium ignites in the core (three dots-dashed line) and when the central helium abundance is 67% (long dashed-line).
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fg11.eps} \end{figure}$	Figure 11: Specific angular momentum profiles of the secondary star on the hydrogen ZAMS (long dashed line), after fast (dotted line) and slow (short dashed line) Case A mass transfer, after Case AB mass transfer (dash-dotted line), when helium ignites in the core (three dots-dashed line) and when the central helium abundance is 67% (solid line).
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fg12.eps} \end{figure}$	Figure 12: Logarithm of the integrated angular momentum J(m)= $\int_{0}^{M}j(m^{\prime}){\rm d}m^{\prime}$ divided by m^5/3, as a function of the mass coordinate m for a 33 $~{M}_{\odot}$ secondary star for the same evolutionary stages as shown in Fig. 11. The thin lines give a logarithmic scale of levels of constant J labeled with $\log(J/\rm (erg~s))$ .
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$\begin{figure} \par\includegraphics[width=8.8cm]{2545fg13.eps} \end{figure}$	Figure 13: Specific angular momentum profiles of the secondary star on the hydrogen ZAMS (solid line) and when helium ignites in the core ( $T_{\rm c}=1.4\times 10^8 \rm ~K$ ), assuming the accretion of 0.25 $~{M}_{\odot}$ (dotted line) 1.4 $~{M}_{\odot}$ (dashed line) or 5 $~{M}_{\odot}$ (dot-dashed line) during Case AB mass transfer.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fg14.eps} \end{figure}$	Figure 14: Specific angular momentum profiles of the 42 $~{M}_{\odot}$ single star with magnetic fields on the hydrogen ZAMS (dot-dashed line), when 50% of hydrogen is left in the center (dotted line), when hydrogen is exhausted in the core (dashed line) and when central helium burning starts (solid line).
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fg15.eps} \end{figure}$	Figure 15: Spin period profiles of the 42 $~{M}_{\odot}$ single star on the ZAMS (solid line), when 50% hydrogen is left in the center (dotted line), when hydrogen is exhausted in the core (dashed line), and when central helium burning starts (dot-dashed line).
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fg16.eps} \end{figure}$	Figure 16: Stellar wind mass loss of the magnetic (dotted line) and non-magnetic (solid line) 42 $~{M}_{\odot}$ star. The star with magnetic fields loses more mass because magnetic torques transport angular momentum, which spins-up the surface layers and enhances mass loss.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fg17.eps} \end{figure}$	Figure 17: Effective viscosities due to magnetic torques (solid line) and due to rotational instabilities (dotted line) for a rotating 42 $~{M}_{\odot}$ star at a central hydrogen abundance of 50% and at core hydrogen exhaustion.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fg18.eps} \end{figure}$	Figure 18: Evolution of the internal structure of a rotating 33 $~{M}_{\odot}$ secondary star with magnetic field from the ZAMS until red supergiant phase $Y_{\rm c}=0.92$ . See Fig. 7 for an explanation of the different hatching types.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fg19.eps} \end{figure}$	Figure 19: Evolution of the internal structure of a rotating 33 $~{M}_{\odot}$ secondary star with magnetic field from after the SN explosion of the primary and disruption of the system. See Fig. 7 for an explanation of the different hatching types.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{2545fg20.eps} \end{figure}$	Figure 20: Specific angular momentum profiles of the secondary star with magnetic fields on the hydrogen ZAMS (long dashed line), after fast (dotted line) and slow (short dashed line) Case A mass transfer, when all hydrogen is exhausted in the center (dot-dashed line), when helium ignites (three dots-dashed line) and and when the central helium abundance is 92% (solid line).
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2545fg21.eps} \end{figure}$	Figure 21: Evolution of the internal structure of a rotating 33 $~{M}_{\odot}$ secondary star until helium ignition in the core. The star accretes 2 $~{M}_{\odot}$ when the central helium abundance is 95%. See Fig. 7 for an explanation of the different hatching types.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{2545fg22.eps} \end{figure}$	Figure 22: Evolution of the internal structure of a rotating 33 $~{M}_{\odot}$ secondary star with magnetic field until helium ignition in the core. The star accretes 2 $~{M}_{\odot}$ when the central helium abundance is 95%. See Fig. 7 for an explanation of the different hatching types.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2545fg23.eps} \end{figure}$	Figure 23: Specific angular momentum profiles of a 33 $~{M}_{\odot}$ non-magnetic star on the ZAMS (long dashed line), when $Y_{\rm c}=95$ % (dotted line), at the end of the accretion (dashed line), 10 $^4\rm ~yr$ after the accretion (dot-dashed line), when hydrogen is exhausted in the core (three dot-dashed line) and when helium ignites in the core (solid line).
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{2545fg24.eps} \end{figure}$	Figure 24: Specific angular momentum profiles of a 33 $~{M}_{\odot}$ magnetic star on the ZAMS (long dashed line), when $Y_{\rm c}=95$ % (dotted line), at the end of the accretion (dashed line), 10 $^4\rm ~yr$ after the accretion (dot-dashed line), when hydrogen is exhausted in the core (three dot-dashed line) and when helium ignites in the core (solid line).
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