All Figures

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1949fig1.eps} \end{figure}$ Figure 1: Plot of the value of the dredge-up parameter $\lambda$ versus the maximum luminosity of the helium shell during a thermal pulse. The data points are taken from Table 1 of Herwig (2000). The straight line is a fit to value of lambda in pulses 4-10.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.3cm,clip]{1949fig2.eps} \end{figure}$ Figure 2: The circles and squares represent the KB and KH data sets, respectively. Open and closed symbols respectively indicate PNe with N/O $\le$ 0.5 and N/O > 0.5, respectively. The solid, dashed, long-dashed, and dash-dotted lines refer to models calculated respectively with [Fe/H] = 0.0, 0.1, 0.2, and -0.5. The mixing length parameter, $\alpha$ , of each model was set to 2.3. Only models with $M<4.6~M_{\odot}$ are shown for the [Fe/H] = 0.2 and only models with $M<2~M_{\odot}$ are shown for the [Fe/H] = -0.5. The solid diamonds indicate the results of models with [Fe/H] = 0.0 and masses of 1.0, 1.6, 2.5, 4.0, 4.1, 6.0, and 8.0 $M_{\odot }$ . Also the position of the model with [Fe/H] = 0.2 and mass of 4.6 $M_{\odot }$ is indicated.
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In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1949fig3.eps} \end{figure}$ Figure 3: The symbols have the same meaning as Fig. 2. The dashed line are the [Fe/H] = 0.1 models.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12.5cm,clip]{1949fig4.eps} \end{figure}$ Figure 4: Total yields of $^{12}\rm C$ , $^{13}\rm C$ , $^{14}\rm N$ and $^{16}\rm O$ produced by LIM stars for different metallicities following label in panel d), expressed as $\log{(Z/Z_{\odot})}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=12cm,clip]{1949fig5.eps} \end{figure}$ Figure 5: Total yields of $^{12}\rm C$ , $^{13}\rm C$ , $^{14}\rm N$ and $^{16}\rm O$ produced by LIM stars of solar composition in this work, called BU, compared with those given by RV, VG, MA, VE and DR marked with different symbols according panel d).
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1949fig6.eps} \end{figure}$ Figure 6: Time evolution in the Solar Vicinity: a) the star formation history and b) the age-metallicity relation. Data are from Twarog (1980) (TWA), Barry (1988) (BA), Edvardsson et al. (1993) (EDV), Carraro et al. (1998) (CAR), Rocha-Pinto et al. (2000a,b) (RO) and Reddy et al. (2003).
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1949fig7.eps} \end{figure}$ Figure 7: G-dwarf distribution for our model compared with data from Chang et al. (2000); Kotoneva et al. (2002) in a) and with data from Jørgensen (2000) in b).
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{1949fig8.eps} \end{figure}$ Figure 8: Time evolution of abundances in the Solar Vicinity: a) oxygen; b) carbon, as $12+\rm log~(X/H)$ ; and c) the ratio C/O. Solar abundances are the filled symbols from Grevesse & Sauval (1998) - circles, Holweger (2001) - squares - and (Allende Prieto et al. 2001a,b, 2002), - crosses, by assuming an age of 4.5 Gyr for the sun. Empty symbols at 13.2 Gyr are the interstellar medium abundances given by Meyer et al. (1997); Meyer et al. (1998), - circles, Peimbert (1999) - squares, Sofia et al. (2001), - triangles, and Moos et al. (2002), - stars. Small open dots are stellar abundances obtained from Table 3, being those located around the Solar Vicinity (7 < R < 9 kpc). Line meanings are given in panel b) of Fig. 6.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{1949fig9.eps} \end{figure}$ Figure 9: Radial distributions of elemental abundances, as 12 + log (X/H), in the Galaxy disk for: a) oxygen; b) carbon and the relative abundance log (C/O). Stellar data - filled dots - are taken from authors given in Table 3. H II regions abundances are also included, taken from Peimbert (1979) - PE, Shaver et al. (1983) - SHA, Fich & Silkey (1991) - FS, Vílchez & Esteban (1996) - VIES, Afflerbach et al. (1997) - AFF, and Esteban et al. (1999ab,c) - EST - as marked in the figure.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.8cm,clip]{1949fig10.eps} \end{figure}$ Figure 10: The relative abundances of log (C/O) vs. the oxygen abundance as $\rm 12+log~(O/H)$ . Stellar data - open circles - are from Table 3. Other data are from Esteban et al. (1999a) - EST99, Tsamis et al. (2003) - TSA, for galactic H II regions, from Garnett et al. (1995,1999) - GR95/99, for other galaxies H II regions and from Izotov & Thuan (1999) - IZ, for Blue compact dwarf galaxies. The meaning of symbols is given in the figure.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{1949fig11.eps} \end{figure}$ Figure 11: The relative abundances of C and O as [X/Fe] vs. the iron abundance [Fe/H]. Panel a) shows the [O/Fe] evolution for the disk. The dot-long-dashed line represents the trend of Boesgaard et al. (1999) data. Panels b) and c) represent the evolution of [C/Fe] for the disk and the halo, respectively. Models have the same line coding as previous figures. Data are taken from authors from Table 3. Open dots are the available data, while solid dots are stars that have known galactocentric distance in the range $7 \le R \le 9$ kpc. Triangles are data from Carbon et al. (1987).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1949fig1.eps} \end{figure}$	Figure 1: Plot of the value of the dredge-up parameter $\lambda$ versus the maximum luminosity of the helium shell during a thermal pulse. The data points are taken from Table 1 of Herwig (2000). The straight line is a fit to value of lambda in pulses 4-10.
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$\begin{figure} \par\includegraphics[width=8.3cm,clip]{1949fig3.eps} \end{figure}$	Figure 3: The symbols have the same meaning as Fig. 2. The dashed line are the [Fe/H] = 0.1 models.
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$\begin{figure} \par\includegraphics[angle=-90,width=12.5cm,clip]{1949fig4.eps} \end{figure}$	Figure 4: Total yields of $^{12}\rm C$ , $^{13}\rm C$ , $^{14}\rm N$ and $^{16}\rm O$ produced by LIM stars for different metallicities following label in panel d), expressed as $\log{(Z/Z_{\odot})}$ .
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$\begin{figure} \par\includegraphics[angle=-90,width=12cm,clip]{1949fig5.eps} \end{figure}$	Figure 5: Total yields of $^{12}\rm C$ , $^{13}\rm C$ , $^{14}\rm N$ and $^{16}\rm O$ produced by LIM stars of solar composition in this work, called BU, compared with those given by RV, VG, MA, VE and DR marked with different symbols according panel d).
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{1949fig6.eps} \end{figure}$	Figure 6: Time evolution in the Solar Vicinity: a) the star formation history and b) the age-metallicity relation. Data are from Twarog (1980) (TWA), Barry (1988) (BA), Edvardsson et al. (1993) (EDV), Carraro et al. (1998) (CAR), Rocha-Pinto et al. (2000a,b) (RO) and Reddy et al. (2003).
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{1949fig7.eps} \end{figure}$	Figure 7: G-dwarf distribution for our model compared with data from Chang et al. (2000); Kotoneva et al. (2002) in a) and with data from Jørgensen (2000) in b).
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