All Figures

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{6363fig1.eps} \end{figure}$ Figure 1: The temporal evolution of the surface density of mass in the gas phase as a function of the distance from the star.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{6363fig2.eps} \end{figure}$ Figure 2: Outward drift velocity of particles as a function of the radial distance from the star, if a disk of age 0.2 Myr were completely transparent. The curves represent particles of different sizes. From bottom to top, the solid curves denote particles of $a=1, 10, 100~\rm \mu m$ , and $a=1~\rm mm$ . The dashed lines are for particles of $a=1~\rm cm$ and $a=3~\rm cm$ . The value for 3 cm particles turns negative inside approximately 0.4 AU. For particles larger than 1 mm the drift velocity also becomes negative beyond 40 AU.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{6363fig3.eps} \end{figure}$ Figure 3: Particle drift and turbulent diffusion at 0.2 Myr. As in Fig. 2 from bottom to top, the solid curves denote particles of $a=1, 10, 100~\rm \mu m$ , and $a=1~\rm mm$ . The dashed and dash-dotted line are for particles of $a=1~\rm cm$ and $a=3~\rm cm$ , respectively. A constant turbulent inward diffusion of 5 m s^-1 has been subtracted for all particle sizes.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{6363fig4.eps} \end{figure}$ Figure 4: a) The position of the inner edge of the dust disk as a function of time for different particle growth timescales. For the solid lines, the growth timescale is t₀ = 100 000 yr, t₀ = 250 000 yr, and t₀ = 500 000 yr (moving from left to right), and $\lambda _{\rm p} = 0.01$ $\rm W~m^{-1}~K^{-1}$ . The dashed line is for t₀ = 250 000 yr and $\lambda _{\rm p} = 0.005$ $\rm W~m^{-1}~K^{-1}$ . The evolution is divided into 3 parts. With increasing time, these parts correspond to slow drift, fast drift, and an inward retreat. b) Corresponding particle size evolution. The growth is cut-off once the particles have reached a size of 1cm. Comparison with a) shows that the edge only starts to move outwards efficiently once particles have grown to $10~\rm \mu m$ or larger.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{6363fig5.eps} \end{figure}$ Figure 5: Same as Fig. 4a but assuming 5 m s^-1 offset due to turbulent diffusion.
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In the text

$\begin{figure} \par\includegraphics[width=7.65cm,clip]{6363fig6.eps} \end{figure}$ Figure 6: Equilibrium position as a function of the minimum particle size for a turbulent disk at the age of 0.2 Myr (solid line) and 3.4 Myr (dashed line).
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In the text

$\begin{figure} \par\includegraphics[width=6.5cm,clip]{6363fig1.eps} \end{figure}$	Figure 1: The temporal evolution of the surface density of mass in the gas phase as a function of the distance from the star.
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$\begin{figure} \par\includegraphics[width=7.65cm,clip]{6363fig3.eps} \end{figure}$	Figure 3: Particle drift and turbulent diffusion at 0.2 Myr. As in Fig. 2 from bottom to top, the solid curves denote particles of $a=1, 10, 100~\rm \mu m$ , and $a=1~\rm mm$ . The dashed and dash-dotted line are for particles of $a=1~\rm cm$ and $a=3~\rm cm$ , respectively. A constant turbulent inward diffusion of 5 m s^-1 has been subtracted for all particle sizes.
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$\begin{figure} \par\includegraphics[width=7.65cm,clip]{6363fig5.eps} \end{figure}$	Figure 5: Same as Fig. 4a but assuming 5 m s^-1 offset due to turbulent diffusion.
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$\begin{figure} \par\includegraphics[width=7.65cm,clip]{6363fig6.eps} \end{figure}$	Figure 6: Equilibrium position as a function of the minimum particle size for a turbulent disk at the age of 0.2 Myr (solid line) and 3.4 Myr (dashed line).
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