Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{3261f1.eps} \end{figure}$ Figure 1: Internal distribution of the angular velocity $\Omega (r)$ as a function of the Lagrangian mass in solar units in a 15 $M_\odot$ model, without magnetic fields, at various stages of the model evolution indicated by the central H-content $X_{{\rm c}}$ during the MS-phase. The initial velocity $\upsilon _{\rm ini} = 300$ km s^-1.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3261f2.eps} \end{figure}$ Figure 2: Same as in Fig. 1 but with magnetic fields. One notices the almost constant values of the angular velocity in the models.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3261f3.eps} \end{figure}$ Figure 3: Evolution of the rotation velocities at the surface of 15 $M_\odot$ models during the MS phase with and without magnetic fields H. The initial velocity $\upsilon _{\rm ini} = 300$ km s^-1 in both cases. We see the much higher surface rotation when magnetic field is included.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3261f4.eps} \end{figure}$ Figure 4: Distribution of the magnetic field in the model of initial 15 $M_\odot$ when the central hydrogen content is $X_{{\rm c}}=0.60$ . The age of the model is $4.2798 \times 10^6$ yr and the actual mass is 14.97 $M_\odot$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3261f5.eps} \end{figure}$ Figure 5: The diffusion coefficients in the model with central H-content $X_{{\rm c}}=0.60$ . In the outer envelope, where the magnetic field is absent, the transports by shear and by combination of the meridional circulation and horizontal turbulence expressed by $D_{{\rm eff}}$ are present.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3261f6.eps} \end{figure}$ Figure 6: Internal distribution of the hydrogen mass fraction X as a function of the Lagrangian mass in a 15 $M_\odot$ model with rotation at various stages of the model evolution from top to bottom during the MS-phase. Some convective zones appear in the H-shell burning stage at the end of the MS phase.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3261f7.eps} \end{figure}$ Figure 7: Internal distribution of the hydrogen mass fraction X as a function of the Lagrangian mass in the model with magnetic field calculated according to expressions of the present paper at various stages of the model evolution from top to bottom during the MS-phase.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip,angle=0]{3261f8.eps} \end{figure}$ Figure 8: Top lines near 15 $M_\odot$ : evolution of the stellar mass. Lower lines: evolution of the mass of the convective core. The dotted line applies to the model without rotation, the short-broken line to the model with rotation ( $\upsilon _{\rm ini} = 300$ km s^-1) but without magnetic fields, the continuous line to the model with rotation ( $\upsilon _{\rm ini} = 300$ km s^-1) and magnetic fields.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,angle=0]{3261f9.eps} \end{figure}$ Figure 9: Evolutionary tracks in the HR diagram for 15 $M_\odot$ stellar models. The dotted line applies to the model without rotation, the short-broken line to the model with rotation ( $\upsilon _{\rm ini} = 300$ km s^-1) but without magnetic fields, the continuous line to the model with rotation ( $\upsilon _{\rm ini} = 300$ km s^-1) and magnetic fields.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,clip,width=13.4cm]{3261f10.eps} \end{figure}$ Figure 10: Time evolution of the surface helium content $Y_{{\rm s}}$ in mass fraction, of the N/O, N/H and N/C in mass fraction for various models: the dotted line applies to the model without rotation, the short-broken line to the model with rotation ( $\upsilon _{\rm ini} = 300$ km s^-1) but without magnetic fields, the continuous line to the model with rotation ( $\upsilon _{\rm ini} = 300$ km s^-1) and magnetic fields.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3261f1.eps} \end{figure}$	Figure 1: Internal distribution of the angular velocity $\Omega (r)$ as a function of the Lagrangian mass in solar units in a 15 $M_\odot$ model, without magnetic fields, at various stages of the model evolution indicated by the central H-content $X_{{\rm c}}$ during the MS-phase. The initial velocity $\upsilon _{\rm ini} = 300$ km s^-1.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3261f2.eps} \end{figure}$	Figure 2: Same as in Fig. 1 but with magnetic fields. One notices the almost constant values of the angular velocity in the models.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3261f3.eps} \end{figure}$	Figure 3: Evolution of the rotation velocities at the surface of 15 $M_\odot$ models during the MS phase with and without magnetic fields H. The initial velocity $\upsilon _{\rm ini} = 300$ km s^-1 in both cases. We see the much higher surface rotation when magnetic field is included.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3261f4.eps} \end{figure}$	Figure 4: Distribution of the magnetic field in the model of initial 15 $M_\odot$ when the central hydrogen content is $X_{{\rm c}}=0.60$ . The age of the model is $4.2798 \times 10^6$ yr and the actual mass is 14.97 $M_\odot$ .
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3261f5.eps} \end{figure}$	Figure 5: The diffusion coefficients in the model with central H-content $X_{{\rm c}}=0.60$ . In the outer envelope, where the magnetic field is absent, the transports by shear and by combination of the meridional circulation and horizontal turbulence expressed by $D_{{\rm eff}}$ are present.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3261f6.eps} \end{figure}$	Figure 6: Internal distribution of the hydrogen mass fraction X as a function of the Lagrangian mass in a 15 $M_\odot$ model with rotation at various stages of the model evolution from top to bottom during the MS-phase. Some convective zones appear in the H-shell burning stage at the end of the MS phase.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3261f7.eps} \end{figure}$	Figure 7: Internal distribution of the hydrogen mass fraction X as a function of the Lagrangian mass in the model with magnetic field calculated according to expressions of the present paper at various stages of the model evolution from top to bottom during the MS-phase.
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$\begin{figure} \par\includegraphics[width=8cm,angle=0]{3261f9.eps} \end{figure}$	Figure 9: Evolutionary tracks in the HR diagram for 15 $M_\odot$ stellar models. The dotted line applies to the model without rotation, the short-broken line to the model with rotation ( $\upsilon _{\rm ini} = 300$ km s^-1) but without magnetic fields, the continuous line to the model with rotation ( $\upsilon _{\rm ini} = 300$ km s^-1) and magnetic fields.
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