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$\begin{figure} \par\includegraphics[width=16cm,clip]{9893fig1.eps} \end{figure}$ Figure 1: SMC ( left), LMC ( middle), and solar ( right) model with identical input parameters $M = 0.9~M_\odot$ , $T_\star = 2800$ K, $L = 10^{4}~L_\odot$ , P = 600 d, $\Delta v = 5$ km s^-1, $\epsilon _{\rm C}$ / $\epsilon _{\rm O}=1.8$ . Shown is the radial structure at time t=90 P, R₀ being the stellar radius at the start of the calculation t=0 P. The depicted quantities are (left scales) the radial velocity v (solid blue line), the speed of sound c_T (dotted blue lines - in-/outwards, zero line as guide to the eye), the density $\rho$ (solid magenta), the nucleation rate per hydrogen atom $J_\star/n_{\langle {\rm H} \rangle}$ (solid black), and the degree of condensation $f_{\rm c}$ of the dust (solid red), (right scales) the gas temperature (dashed red) and equilibrium temperature (solid cyan) T, the ratio of radiative to gravitational acceleration $\alpha$ of the material (dashed blue), the dust density $n_{\rm d}$ (dashed cyan), and the mean dust particle radius $\langle r \rangle$ (dashed blue).
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In the text

$\begin{figure} {\bf (a)} LMC: \\ [-2ex] {\includegraphics[angle=270,width=8.2cm,... ...-2ex] {\includegraphics[angle=270,width=8.2cm,clip]{9893fi2b.ps} } \end{figure}$ Figure 2: Graphical illustration of the fit formulae for the mass loss rate for fixed mass $M_\star = 1.0~M_\odot$ .
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In the text

$\begin{figure} \mbox{\hspace*{0.5cm}{{\bf (a)} $Z = 0.01$ , $M_{\rm i} = 1.25 ~ ... ...{3mm} \includegraphics[angle=270,width=8.5cm,clip]{9893fi3d.ps} } \end{figure}$ Figure 3: Mass loss histories of stars with different initial masses and metallicities. Labels denote the current mass.
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In the text

$\begin{figure} {\small {\bf (a)} Models with metallicity $Z=0.01$ :}\\ [-1ex] {... ...-1ex] {\includegraphics[angle=270,width=8.2cm,clip]{9893fi4b.ps} } \end{figure}$ Figure 4: Integrated mass loss as a function of initial mass. For each initial mass the total mass loss is shown (blue diamonds) as well as the respective fractions lost on the RGB (cyan) and the AGB (grey). For reference the respective solar values are given as well in both plots (red, green, and black crosses).
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In the text

$\begin{figure} {\bf (a)} LMC: \\ [-2ex] {\includegraphics[angle=270,width=8.2cm,... ...-2ex] {\includegraphics[angle=270,width=8.2cm,clip]{9893fi2b.ps} } \end{figure}$	Figure 2: Graphical illustration of the fit formulae for the mass loss rate for fixed mass $M_\star = 1.0~M_\odot$ .
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$\begin{figure} \mbox{\hspace*{0.5cm}{{\bf (a)} $Z = 0.01$ , $M_{\rm i} = 1.25 ~ ... ...{3mm} \includegraphics[angle=270,width=8.5cm,clip]{9893fi3d.ps} } \end{figure}$	Figure 3: Mass loss histories of stars with different initial masses and metallicities. Labels denote the current mass.
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$\begin{figure} {\small {\bf (a)} Models with metallicity $Z=0.01$ :}\\ [-1ex] {... ...-1ex] {\includegraphics[angle=270,width=8.2cm,clip]{9893fi4b.ps} } \end{figure}$	Figure 4: Integrated mass loss as a function of initial mass. For each initial mass the total mass loss is shown (blue diamonds) as well as the respective fractions lost on the RGB (cyan) and the AGB (grey). For reference the respective solar values are given as well in both plots (red, green, and black crosses).
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