Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1692fig1.eps} \end{figure}$ Figure 1: The probability of planet occurrence as a function of the star's iron abundance (on the standard logarithmic scale with zero representing the solar value). Reproduced with permission from Fischer & Valenti (2003).
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1692fig2.ps} \end{figure}$ Figure 2: The rate of planet occurrence as a function of the primordial metallicity of protoplanetary disks. Lines marked with different symbols are obtained for different values of $\alpha$ , as labeled in the upper left corner. Filled symbols: models with the redistribution of solids; open symbols: models with a constant $\Sigma _{\rm s}/\Sigma _{\rm g}$ ratio. The histogram shows the observational data.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1692fig3.eps} \end{figure}$ Figure 3: As functions of the initial disk mass M₀ (in solar masses) and the logarithm of the initial radius R₀ in astronomical units, the contours and grey scale, respectively, give the inner and outer radius of the region around the central star where giant planet formation is possible in a maximum of 3 Myr. White circles indicate disk models where the solid surface density is everywhere below the critical value for planet formation. Black circles indicate disks in which all of the solid material accretes onto the star. The disk viscosity parameter is $\alpha = 1 \times 10^{-2}$ , and the primordial metallicity is solar.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1692fig4.ps} \end{figure}$ Figure 4: Rate of planet occurrence as a function of the primordial metallicity in models with the redistribution of solids included. Same as in Fig. 2, but all curves are normalized to match the observational data for $\lg Z = 0.48$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1692fig5.ps} \end{figure}$ Figure 5: Rate of planet occurrence as a function of the primordial metallicity in models without the redistribution of solids. Same as in Fig. 2, but all curves are normalized to match the observational data for $\lg Z = 0.48$ .
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1692fig6.ps} \end{figure}$ Figure 6: Same as Fig. 4, but based on disk models with initial parameters uniformly distributed on the $[M_0,\lg j_0]$ plane.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1692fig1.eps} \end{figure}$	Figure 1: The probability of planet occurrence as a function of the star's iron abundance (on the standard logarithmic scale with zero representing the solar value). Reproduced with permission from Fischer & Valenti (2003).
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1692fig4.ps} \end{figure}$	Figure 4: Rate of planet occurrence as a function of the primordial metallicity in models with the redistribution of solids included. Same as in Fig. 2, but all curves are normalized to match the observational data for $\lg Z = 0.48$ .
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1692fig5.ps} \end{figure}$	Figure 5: Rate of planet occurrence as a function of the primordial metallicity in models without the redistribution of solids. Same as in Fig. 2, but all curves are normalized to match the observational data for $\lg Z = 0.48$ .
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$\begin{figure} \par\includegraphics[angle=-90,width=8cm,clip]{1692fig6.ps} \end{figure}$	Figure 6: Same as Fig. 4, but based on disk models with initial parameters uniformly distributed on the $[M_0,\lg j_0]$ plane.
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