$\begin{figure} \par\includegraphics[width=8.8cm,clip]{anavsnum.eps} \end{figure}$ Figure 1: Relative shift $\delta R/R_*$ of the effective ILRs and OLRs due to the disk mass, for the following parameters: $a_{\rm in}=0.01$ , $a_{\rm out}=1$ , $\mu =0.05$ and $R_{\rm pl}/a_{\rm out}=~0.5$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{torque005.eps} \end{figure}$ Figure 2: Inner and outer Lindblad torques ( left) and differential torques ( right) when the disk mass is accounted for, compared to the case without disk gravity. The conditions are the same as for Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{vss.xfig.eps} \end{figure}$ Figure 3: Relative shifts of the OLRs and ILRs ( left) and differential Lindblad ( right) for different power law surface density profiles (see text). The conditions are the same as for Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{mig.xfig.eps} \end{figure}$ Figure 4: Total differential torque versus the planet position relative to the outer edge for $\mu =0.05$ ( left), and versus the relative disk mass $\mu$ for $R_{\rm pl}=0.5$ ( right), for different power law surface density profile in the disk (see text).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{anavsnum.eps} \end{figure}$	Figure 1: Relative shift $\delta R/R_*$ of the effective ILRs and OLRs due to the disk mass, for the following parameters: $a_{\rm in}=0.01$ , $a_{\rm out}=1$ , $\mu =0.05$ and $R_{\rm pl}/a_{\rm out}=~0.5$ .
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{torque005.eps} \end{figure}$	Figure 2: Inner and outer Lindblad torques ( left) and differential torques ( right) when the disk mass is accounted for, compared to the case without disk gravity. The conditions are the same as for Fig. 1.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{vss.xfig.eps} \end{figure}$	Figure 3: Relative shifts of the OLRs and ILRs ( left) and differential Lindblad ( right) for different power law surface density profiles (see text). The conditions are the same as for Fig. 1.
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$\begin{figure} \par\includegraphics[width=8.6cm,clip]{mig.xfig.eps} \end{figure}$	Figure 4: Total differential torque versus the planet position relative to the outer edge for $\mu =0.05$ ( left), and versus the relative disk mass $\mu$ for $R_{\rm pl}=0.5$ ( right), for different power law surface density profile in the disk (see text).
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