All Figures

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{7950fig1.eps} \end{figure}$ Figure 1: Evolution of the gas surface density within the inner 10 AU of our simulated disk. The upper line is the initial $r^{-1.5}~\Sigma_{\rm g}$ -profile for a $3 \times {\rm MMSN}$ disk. The lower curves, in descending order, are the profiles at 0.1, 1.0 and 1.5 Myr respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{7950fig2.eps} \end{figure}$ Figure 2: Protoplanetary masses vs. semi-major axis obtained after evolution to the starting points of scenarios I, IV and V. Substantial inward drift is visible at late times due to type I migration.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{7950fig3.eps} \end{figure}$ Figure 3: Scenario IV at 20 000 years after the start of giant planet migration, showing the mass, inclination and eccentricity of objects. Small black dots represent super-planetesimals; white filled circles are rocky protoplanets; grey filled circles are icy protoplanets and the large highlighted grey filled circle is the giant. Objects plotted between the dotted lines in the upper panel have orbits that intersect the orbit of the giant. The location of the 2:1, 3:2 and 4:3 resonances with the giant are indicated. Gas surface density is read on the right hand axis of the lower panel, the upper grey curve being the unevolved profile at t = 0 and the lower black curve being the current profile.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{7950fig4.eps} \end{figure}$ Figure 4: Scenario IV at 80 000 years after the start of giant planet migration. The giant has now moved inward to 2.04 AU and is beginning to enter the inner zone that has become packed with protoplanets due to previous type I migration.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{7950fig5.eps} \end{figure}$ Figure 5: Scenario IV at 120 000 years after the start of giant planet migration. The giant has now moved inward to 0.72 AU. Six more protoplanets and a substantial number of planetesimals have been scattered into the external disk.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{7950fig6.eps} \end{figure}$ Figure 6: The end point of scenario IV at 152 500 years after the start of giant planet migration. The giant is at 0.1 AU. About half of the original solids disk mass survives in external orbits and seven protoplanets are found between 0.7-3 AU. A hot-Earth remains interior to the giant planet in an eccentric and inclined orbit.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{7950fig7.eps} \end{figure}$ Figure 7: Scenario IV interior to 3 AU at the point where the giant planet reaches 0.1 AU. Inclination is plotted vs. semi-major axis. Super planetesimals are the grey dots and protoplanets the open circles. Planets also have marked their masses in ${M}_\oplus$ and their radial excursions due to orbital eccentricity.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{7950fig8.eps} \end{figure}$ Figure 8: Mass fractions of scattered disks generated in the present work compared to those of analogous scenarios not including type I migration and before and after protoplanet mass fractions.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{7950fig9.eps} \end{figure}$ Figure 9: Details of the inner 3 AU at the end of scenario IV ( top panel) and 1.3475 Myr later at the point of gas dispersal. Eccentricity is plotted against semi-major axis with orbital excursions due to eccentricity illustrated with error bars. Planetary masses are labeled in units of ${M}_\oplus$ . $\Sigma _{\rm g}$ is read from the right hand axes: the upper curve being the profile at t = 0 (system age = 0.5 Myr) and the lower curve being the present profile. The extent of the maximum greenhouse habitable zone (0.8-1.7 AU) is shown by the horizontal bar.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{7950fig10.eps} \end{figure}$ Figure 10: Resonant angles for the 5:2 mean motion resonance between the giant planet and the innermost external protoplanet. Resonant capture is indicated $\sim$ 125 000 years before the stage shown in the bottom panel of Fig. 9.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{7950fig11.eps} \end{figure}$ Figure 11: Material composition of protoplanets in the extended scenario IV at the stage shown in the bottom panel of Fig. 9.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{7950fig12.eps} \end{figure}$ Figure 12: Details of the inner 3 AU of the Scenario IV system after 3 Myr of gas-free dynamics. The top and bottom panels show configurations at system ages of 4 and 6 Myr respectively.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{7950fig13.eps} \end{figure}$ Figure 13: Further evolution of the orbits of the interior planets resulting from the three scenarios. Solid lines are semi-major axes, dotted lines are periastra and apastra. Black represents the giant planet and grey represents the hot-Earth.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{7950fig14.eps} \end{figure}$ Figure 14: Hot-Earth-hot-Jupiter systems resulting from an additional 10 000 years of simulation. Error bars show the radial distance between periastron and apastron. Numeric labels give masses in ${M}_\oplus$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{7950fig1.eps} \end{figure}$	Figure 1: Evolution of the gas surface density within the inner 10 AU of our simulated disk. The upper line is the initial $r^{-1.5}~\Sigma_{\rm g}$ -profile for a $3 \times {\rm MMSN}$ disk. The lower curves, in descending order, are the profiles at 0.1, 1.0 and 1.5 Myr respectively.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{7950fig2.eps} \end{figure}$	Figure 2: Protoplanetary masses vs. semi-major axis obtained after evolution to the starting points of scenarios I, IV and V. Substantial inward drift is visible at late times due to type I migration.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{7950fig4.eps} \end{figure}$	Figure 4: Scenario IV at 80 000 years after the start of giant planet migration. The giant has now moved inward to 2.04 AU and is beginning to enter the inner zone that has become packed with protoplanets due to previous type I migration.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{7950fig5.eps} \end{figure}$	Figure 5: Scenario IV at 120 000 years after the start of giant planet migration. The giant has now moved inward to 0.72 AU. Six more protoplanets and a substantial number of planetesimals have been scattered into the external disk.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{7950fig6.eps} \end{figure}$	Figure 6: The end point of scenario IV at 152 500 years after the start of giant planet migration. The giant is at 0.1 AU. About half of the original solids disk mass survives in external orbits and seven protoplanets are found between 0.7-3 AU. A hot-Earth remains interior to the giant planet in an eccentric and inclined orbit.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{7950fig7.eps} \end{figure}$	Figure 7: Scenario IV interior to 3 AU at the point where the giant planet reaches 0.1 AU. Inclination is plotted vs. semi-major axis. Super planetesimals are the grey dots and protoplanets the open circles. Planets also have marked their masses in ${M}_\oplus$ and their radial excursions due to orbital eccentricity.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{7950fig8.eps} \end{figure}$	Figure 8: Mass fractions of scattered disks generated in the present work compared to those of analogous scenarios not including type I migration and before and after protoplanet mass fractions.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{7950fig10.eps} \end{figure}$	Figure 10: Resonant angles for the 5:2 mean motion resonance between the giant planet and the innermost external protoplanet. Resonant capture is indicated $\sim$ 125 000 years before the stage shown in the bottom panel of Fig. 9.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{7950fig11.eps} \end{figure}$	Figure 11: Material composition of protoplanets in the extended scenario IV at the stage shown in the bottom panel of Fig. 9.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{7950fig12.eps} \end{figure}$	Figure 12: Details of the inner 3 AU of the Scenario IV system after 3 Myr of gas-free dynamics. The top and bottom panels show configurations at system ages of 4 and 6 Myr respectively.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{7950fig13.eps} \end{figure}$	Figure 13: Further evolution of the orbits of the interior planets resulting from the three scenarios. Solid lines are semi-major axes, dotted lines are periastra and apastra. Black represents the giant planet and grey represents the hot-Earth.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{7950fig14.eps} \end{figure}$	Figure 14: Hot-Earth-hot-Jupiter systems resulting from an additional 10 000 years of simulation. Error bars show the radial distance between periastron and apastron. Numeric labels give masses in ${M}_\oplus$ .
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