Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{0036fig1.ps} \end{figure}$ Figure 1: The evolution of solids in an $\alpha = 0.1$ disk with m₀ = 0.02 and j₀ = 1. Top: surface density of solids at the times indicated in the frame (solids that have sublimated but not yet accreted onto the star are not taken into account). Bottom: locations of sublimation limit (dashed) and snowline (solid) as a function of time The snowline is defined as the inner edge of the region where ice grains are present.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{aa0036f2.eps} \end{figure}$ Figure 2: The decimal logarithm of surface density enhancement $\xi _{\rm s}$ , defined by Eq. (1) for models with $\alpha = 0.001$ ( left) and $\alpha = 0.1$ ( right). The values of $\log \xi_{\rm s}$ are plotted on the plane of m₀ and j₀ (the initial values of mass and angular momentum of the disk). Within the light-gray region at the lower right corner of each frame the solid component has completely accreted onto the star. The step-like shape of the boundary of that region results from insufficient resolution of the grid (the locations of our models are indicated by dots).
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0036fig3.ps} \end{figure}$ Figure 3: Correlation between the final location of the snowline $R_{\rm sl}^{\rm f}$ and the distance $R_{\rm evap}^{\rm K}$ at which "Keplerian particles'' appear at the sublimation limit. Points with error bars indicate the location of our disk models on the ( $R_{\rm sl}$ , $R_{\rm evap}^{\rm K}$ ) plane. The length of the error bars is equal to the local grid spacing in r In the lower frame $R_{\rm sl}^{\rm f}$ is smaller because disks with smaller $\alpha$ are cooler.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0036fig4.ps} \end{figure}$ Figure 4: The evolution of solids in an $\alpha = 0.001$ disk with m₀ = 0.2and j₀ = 9. Top: surface density of solids at the times indicated in the frame. Bottom: final distributions of solids obtained for the indicated vaules of the coagulation efficiency parameter $\epsilon$ .
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0036fig4.ps} \end{figure}$	Figure 4: The evolution of solids in an $\alpha = 0.001$ disk with m₀ = 0.2and j₀ = 9. Top: surface density of solids at the times indicated in the frame. Bottom: final distributions of solids obtained for the indicated vaules of the coagulation efficiency parameter $\epsilon$ .
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