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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{Maederf1.eps}\end{figure}$ Figure 1: Evolution as a function of the remaining mass of the surface abundances in mass fraction for a 60 $M_\odot$ stellar model at Z=10^-5 and with $\upsilon _{\rm ini}=800$ km s^-1, i.e. an initial ratio of angular velocity to the critical value $\Omega /\Omega _{{\rm c}}=0.85$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{Maederf2.eps}\end{figure}$ Figure 2: Variations of the abundances (in mass fraction) as a function of the Lagrangian mass for ( left) a 7 $M_\odot$ stellar model in the early AGB phase, and for ( right) a 60 $M_\odot$ model at the end of the core C-burning phase. Both models were computed with $\upsilon _{\rm ini}$ = 800 km s^-1 corresponding respectively to $\Omega /\Omega _{{\rm c}}=0.83$ and 0.85. Both models have Z=10^-5.
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In the text

$\begin{figure} \par\includegraphics[height=5.4cm,width=8.3cm,clip]{Maederf3.eps}\end{figure}$ Figure 3: Variations for a 60 $M_\odot$ model with initial $\Omega /\Omega _{{\rm c}}=0.85$ and Z=10^-5: left) the ratio $\Delta Y/\Delta Z$ as a function of the ejected mass; right) the same for the ratio of nitrogen to oxygen normalized to solar. The continuous line corresponds to the mass ejected by stellar winds, the dashed line shows how the ratios would vary if some amount of mass from the pre-SN model is added to the ejecta. The dotted lines indicate the CNO equilibrium values obtained in the convective core of the star, when the mass fraction of hydrogen at the center is 0.34.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{Maederf1.eps}\end{figure}$	Figure 1: Evolution as a function of the remaining mass of the surface abundances in mass fraction for a 60 $M_\odot$ stellar model at Z=10^-5 and with $\upsilon _{\rm ini}=800$ km s^-1, i.e. an initial ratio of angular velocity to the critical value $\Omega /\Omega _{{\rm c}}=0.85$ .
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