All Figures

$\begin{figure} \par\includegraphics[angle=-90,width=7.55cm,clip]{3689sig.ps}\includegraphics[angle=-90,width=7.45cm,clip]{3689T.ps}\end{figure}$ Figure 1: The initial surface density ( left panel) and temperature ( right panel) as a function of distance from the star in the protoplanetary disk with an initial mass $M_0=0.1~M_\odot$ and outer radius $R_0=1000~{\rm AU}$ . Different curves correspond to different values of the mass of the central star in solar masses as described by the labels.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.35cm,clip]{3689sig_.ps}\end{figure}$ Figure 2: The surface density of solids as a function distance from the star in the protoplanetary disk with the same parameters as in Fig. 1 after $10^6~{\rm yr}$ from the beginning of its evolution. Different curves correspond to different values of the mass of the central star in solar masses as described by the labels.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.25cm,clip]{3689sigc.ps}\end{figure}$ Figure 3: The minimum surface density of a planetesimal swarm needed to from a 1 $M_{\rm J}$ planet in less than 3 $\times$ 10⁶ yr as a function of distance from the central star. Different curves are obtained for different masses of the central star, as labeled in units of solar masses in the upper right corner.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8.25cm,clip]{3689scon.ps}\end{figure}$ Figure 4: The minimum surface density of the planetesimal swarm needed to form a 1 $M_{\rm J}$ planet in less than 3 $\times$ 10⁶ yr as a function of distance from the central star, calculated with a constant value of $C_{\rm cap}=5$ . The solid line represents the results of exact values obtained numerically, while dotted lines represent analytical approximations given by Eqs. (16) and (22). The mass of the central star is $1~M_\odot$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{36891.0_.eps}\end{figure}$ Figure 5: The plane of initial parameters of protoplanetary disk models [M₀, $\log R_0$ ]. Minimum and maximum distance from a $1~M_\odot$ star at which the formation of a 1 $M_{\rm J}$ planet is possible within 3 $\times$ 10⁶ yr is indicated by contours and a grey scale, respectively. White circles indicate disk models in which the surface density of the planetesimal swarm is everywhere lower than the critical value for planet formation. Black circles indicate disks in which all solids are accreted onto the star.
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{36890.5_.eps}\end{figure}$ Figure 6: Same as Fig. 5 but for the central star with a mass of $0.5~M_\odot$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.3cm,clip]{36894.0_.eps}\end{figure}$ Figure 7: Same as Fig. 5 but for the central star with a mass of $4~M_\odot$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm,clip]{3689P_p.ps}\end{figure}$ Figure 8: The rate of planet occurrence as a function of the primordial metallicity of protoplanetary disks. Different lines are obtained for models with different masses of the central star, as labeled in solar units in the upper left corner. The histogram shows the observational data compiled by Fischer & Valenti (2003).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm,clip]{3689P_p_.ps}\end{figure}$ Figure 9: The rate of planet occurrence as a function of the primordial metallicity of protoplanetary disks. Disks around stars with masses of $1~M_\odot$ are represented by a solid line. Disks around stars with masses of $0.5~M_\odot$ are represented by dotted and dashed lines. In the first case the range of initial masses of the disks is the same as in the case of solar type stars, while in the second it was scaled according to the mass of the central star.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=7.55cm,clip]{3689sig.ps}\includegraphics[angle=-90,width=7.45cm,clip]{3689T.ps}\end{figure}$	Figure 1: The initial surface density ( left panel) and temperature ( right panel) as a function of distance from the star in the protoplanetary disk with an initial mass $M_0=0.1~M_\odot$ and outer radius $R_0=1000~{\rm AU}$ . Different curves correspond to different values of the mass of the central star in solar masses as described by the labels.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.35cm,clip]{3689sig_.ps}\end{figure}$	Figure 2: The surface density of solids as a function distance from the star in the protoplanetary disk with the same parameters as in Fig. 1 after $10^6~{\rm yr}$ from the beginning of its evolution. Different curves correspond to different values of the mass of the central star in solar masses as described by the labels.
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$\begin{figure} \par\includegraphics[angle=-90,width=8.25cm,clip]{3689sigc.ps}\end{figure}$	Figure 3: The minimum surface density of a planetesimal swarm needed to from a 1 $M_{\rm J}$ planet in less than 3 $\times$ 10⁶ yr as a function of distance from the central star. Different curves are obtained for different masses of the central star, as labeled in units of solar masses in the upper right corner.
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{36890.5_.eps}\end{figure}$	Figure 6: Same as Fig. 5 but for the central star with a mass of $0.5~M_\odot$ .
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$\begin{figure} \par\includegraphics[width=7.3cm,clip]{36894.0_.eps}\end{figure}$	Figure 7: Same as Fig. 5 but for the central star with a mass of $4~M_\odot$ .
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$\begin{figure} \par\includegraphics[angle=-90,width=7.7cm,clip]{3689P_p.ps}\end{figure}$	Figure 8: The rate of planet occurrence as a function of the primordial metallicity of protoplanetary disks. Different lines are obtained for models with different masses of the central star, as labeled in solar units in the upper left corner. The histogram shows the observational data compiled by Fischer & Valenti (2003).
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