All Figures

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7789f1.eps}\end{figure}$ Figure 1: Time evolution of the total surface density $\Sigma _{\rm tot}$ (full line), of the surface density of visible stars (dotted line), and of the interstellar matter surface density $\Sigma _{\rm ISM}$ (dashed line) of the galactic disk at the solar distance from the galactic centre, and observed values for the present day total surface density in the solar neighbourhood (Holmberg & Flynn 2004), for the surface density of the stellar component (Gilmore et al. 1989), and for the surface density of the interstellar medium (Dickey 1993).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7789f2.eps}\vspace*{3mm} \includegraphics[width=7.8cm,clip]{7789f3.eps}\end{figure}$ Figure 2: a) Evolution of the astration rate B at the solar galactocentric distance $r_{\odot }$ . The error bar shows the presently observed stellar birthrate (Rana 1991). b) Evolution of the supernova type II (full line) and type Ia (dashed line) rates at the solar galactocentric distance $r_{\odot }$ and observed values at the present time from Tammann (1994).
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{7789f4.eps}\end{figure}$ Figure 3: Evolution of metallicity Z of the ISM at the solar galactocentric distance $r_{\odot }$ and of the [Fe/H] abundance ratio. The error bars show the observed age-metallicity relation from Rocha-Pinto (2000). The thin vertical line indicates the Solar System birth time which we assume to be 4.56 Gyr ago, and the two filled circles indicate the observed metallicity of the sun and of the present-day ISM.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{7789f5.eps}\end{figure}$ Figure 4: G-dwarf metallicity distribution in the solar vicinity predicted by the model and the observed distribution as derived by Nordström (2004). The thin dashed line shows the G-dwarf distribution from direct calculations, while the thick dotted line is the result of a convolution with a Gaussian with half-width 0.2 dex to account for the observational scatter.
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In the text

$\begin{figure} \par\includegraphics[width=11.5cm,clip]{7789f6.eps}\end{figure}$ Figure 5: Comparison of the predicted abundance ratios of the main dust-forming elements [El/Fe] with observations of stellar abundances. The solid and dashed lines show model calculations with Nomoto (2006) and Woosley & Weaver (1995) SNII yields, respectively. We corrected WW95 yields for Fe and Mg to achieve better fits to observations. For illustrative purposes, a model calculation with uncorrected Mg yields from WW95 is shown with a thin dashed line. The observed stellar element abundances for F and G stars from the solar neighbourhood are shown with different symbols for each of the sources (Akerman et al. 2004; Reddy et al. 2003; Soubiran et al. 2005; Melendez et al. 2002; Jonsell et al. 2005; Venn et al. 2004; Chen et al. 2000; Gratton et al. 1991; Caffau et al. 2005; Cayrel et al. 2004).
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{7789f7.eps}\end{figure}$ Figure 6: Abundance ratio Si/Mg of the major silicate dust forming elements. The full line corresponds to a model using SN yields of Nomoto et al. (2006), the dashed line to a model using SN yields from Woosley & Weaver (1995). For the latter the Mg abundance is scaled such that it reproduces the solar Mg abundance at [Fe/H] = 0.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7789f8.eps}\end{figure}$ Figure 7: Calculated element abundances relative to the solar abundances at the instant of Solar System formation (data according to Table 2). Thin dotted lines show the as much as twice a deviation from observed values.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7789f9.eps}\end{figure}$ Figure 8: Calculated element abundances relative to the abundances of F & G stars from the solar vicinity, with ages less than 1 Gyr (pluses), and of B stars from the range $r_{\odot}\pm2~\rm kpc$ of the galactocentric distances (crosses) (data according to Table 3). Thin dotted lines show the as much as twice a deviation from observed values.
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{7789f10.eps}\end{figure}$ Figure 9: Characteristic astration timescale for conversion of interstellar matter into stars at the solar circle.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{7789f11.eps}\hspace*{2cm} ... ...13.eps}\hspace*{2cm} \includegraphics[width=7.3cm,clip]{7789f14.eps}\end{figure}$ Figure 10: Dependence of the dust masses returned by single AGB stars for the four main kinds of dust species (silicates, carbon, silicon carbide, and iron) on metallicity Z and initial stellar mass M_*. All masses are in units of $M_{\odot }$ . Data from Ferrarotti & Gail (2006) with some additional models.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{7789f15.eps}\end{figure}$ Figure 11: Evolution of the dust injection rates at the solar circle from different stellar sources.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7789f16.eps}\end{figure}$ Figure 12: Growth timescale for the dust species growing in molecular clouds for the Milky Way model at the solar circle: silicate dust (full line), carbon dust (dashed line), iron dust (dotted line).
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{7789f17.eps}\end{figure}$ Figure 13: Approximation for the variation of the degree of condensation $f_{\rm ret}$ with $\tau _{\rm gr}/\tau _{\rm exch}$ for f₀=0.3. The full line shows the result of a numerical evaluation of the integral (37), the dashed lines the two limit cases Eqs. (43) and (44), and the dotted line the approximation (45) (the full and dashed lines nearly coincide).
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{7789f18.eps}\end{figure}$ Figure 14: Growth of dust in molecular clouds at the solar circle. Thick lines show f, the average degree of condensation of the key elements into dust for the dust species shown at the instant when the molecular clouds are dispersed and their material is mixed with the other phases of the ISM. Thin lines show f₀, the corresponding degree of condensation at the formation time of clouds. One always has f₀<f since dust grains grow in molecular clouds and are partially destroyed again in the ISM outside of clouds until they enter the next cloud. Growth of iron dust in clouds starts with a significant time delay because of delayed iron production by SN Ia events. The calculation is for $\xi _{\rm CO}= 0.2$ ; the result for $\xi _{\rm CO}=0.4$ is not shown because the corresponding curves are almost the sames.
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In the text

$\begin{figure} \par\includegraphics[width=9.7cm,clip]{7789f19.eps}\end{figure}$ Figure 15: Evolution of the dust mass fraction in the interstellar medium of the main interstellar dust components and of the stardust species at the solar circle. The dust grown in molecular clouds dominates the total dust mass of the interstellar medium. For carbon dust two results are shown corresponding to an assumed fraction of 0.2 resp. 0.4 of the carbon in molecular clouds blocked in the CO molecule.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7789f20.eps}\end{figure}$ Figure 16: Evolution of abundances in dust per million hydrogen atoms of the main dust-forming elements as predicted by the model calculation. Two lines are shown for carbon. The upper one is for the case that a fraction of $\xi _{\rm CO}= 0.2$ of the carbon is bound in the in-reactive molecule CO, the lower one for the case $\xi _{\rm CO}=0.4$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{7789f21.eps}\end{figure}$ Figure 17: Predicted average depletions of main dust-forming elements at the present time are shown with filled circles. Upper and lower points for depletions for carbon calculated with CO mass fraction 0.4 and 0.2 correspondingly. Upper and lower open triangles with error bars represent observed depletions in warm and cold diffuse clouds, respectively, from Welty et al. (1999) for C, Si, Fe and Cartledge et al. (2006) for O and Mg. Filled triangles mark the average depletions in diffuse clouds (see Whittet 2003, and references therein).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7789f22.eps}\end{figure}$ Figure 18: Evolution of the dust-to-gas ratio at the solar circle as predicted by the model calculation.
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In the text

$\begin{figure} \par\includegraphics[width=13.3cm,clip]{7789f23.eps}\end{figure}$ Figure 19: Composition of the interstellar mixture of dust species grown in molecular clouds, the MC-grown dust, and of the presolar dust species from AGB stars and supernovae, the stardust, at the solar circle. Left: at the instant of Solar System formation. Right: for the present solar neighbourhood.
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7789f2.eps}\vspace*{3mm} \includegraphics[width=7.8cm,clip]{7789f3.eps}\end{figure}$	Figure 2: a) Evolution of the astration rate B at the solar galactocentric distance $r_{\odot }$ . The error bar shows the presently observed stellar birthrate (Rana 1991). b) Evolution of the supernova type II (full line) and type Ia (dashed line) rates at the solar galactocentric distance $r_{\odot }$ and observed values at the present time from Tammann (1994).
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{7789f5.eps}\end{figure}$	Figure 4: G-dwarf metallicity distribution in the solar vicinity predicted by the model and the observed distribution as derived by Nordström (2004). The thin dashed line shows the G-dwarf distribution from direct calculations, while the thick dotted line is the result of a convolution with a Gaussian with half-width 0.2 dex to account for the observational scatter.
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$\begin{figure} \par\includegraphics[width=6.5cm,clip]{7789f7.eps}\end{figure}$	Figure 6: Abundance ratio Si/Mg of the major silicate dust forming elements. The full line corresponds to a model using SN yields of Nomoto et al. (2006), the dashed line to a model using SN yields from Woosley & Weaver (1995). For the latter the Mg abundance is scaled such that it reproduces the solar Mg abundance at [Fe/H] = 0.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7789f8.eps}\end{figure}$	Figure 7: Calculated element abundances relative to the solar abundances at the instant of Solar System formation (data according to Table 2). Thin dotted lines show the as much as twice a deviation from observed values.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7789f9.eps}\end{figure}$	Figure 8: Calculated element abundances relative to the abundances of F & G stars from the solar vicinity, with ages less than 1 Gyr (pluses), and of B stars from the range $r_{\odot}\pm2~\rm kpc$ of the galactocentric distances (crosses) (data according to Table 3). Thin dotted lines show the as much as twice a deviation from observed values.
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{7789f10.eps}\end{figure}$	Figure 9: Characteristic astration timescale for conversion of interstellar matter into stars at the solar circle.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{7789f11.eps}\hspace{2cm} ... ...13.eps}\hspace{2cm} \includegraphics[width=7.3cm,clip]{7789f14.eps}\end{figure}$	Figure 10: Dependence of the dust masses returned by single AGB stars for the four main kinds of dust species (silicates, carbon, silicon carbide, and iron) on metallicity Z and initial stellar mass M_*. All masses are in units of $M_{\odot }$ . Data from Ferrarotti & Gail (2006) with some additional models.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{7789f15.eps}\end{figure}$	Figure 11: Evolution of the dust injection rates at the solar circle from different stellar sources.
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7789f16.eps}\end{figure}$	Figure 12: Growth timescale for the dust species growing in molecular clouds for the Milky Way model at the solar circle: silicate dust (full line), carbon dust (dashed line), iron dust (dotted line).
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{7789f17.eps}\end{figure}$	Figure 13: Approximation for the variation of the degree of condensation $f_{\rm ret}$ with $\tau _{\rm gr}/\tau _{\rm exch}$ for f₀=0.3. The full line shows the result of a numerical evaluation of the integral (37), the dashed lines the two limit cases Eqs. (43) and (44), and the dotted line the approximation (45) (the full and dashed lines nearly coincide).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7789f20.eps}\end{figure}$	Figure 16: Evolution of abundances in dust per million hydrogen atoms of the main dust-forming elements as predicted by the model calculation. Two lines are shown for carbon. The upper one is for the case that a fraction of $\xi _{\rm CO}= 0.2$ of the carbon is bound in the in-reactive molecule CO, the lower one for the case $\xi _{\rm CO}=0.4$ .
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{7789f22.eps}\end{figure}$	Figure 18: Evolution of the dust-to-gas ratio at the solar circle as predicted by the model calculation.
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$\begin{figure} \par\includegraphics[width=13.3cm,clip]{7789f23.eps}\end{figure}$	Figure 19: Composition of the interstellar mixture of dust species grown in molecular clouds, the MC-grown dust, and of the presolar dust species from AGB stars and supernovae, the stardust, at the solar circle. Left: at the instant of Solar System formation. Right: for the present solar neighbourhood.
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