All Figures

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{6171fig1.eps} \end{figure}$ Figure 1: Evolution of the mass of the gas disk. The mass of gas (in Jupiter masses) remaining at the launch point for each of the five migration scenarios is indicated.
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In the text

$\begin{figure} \par\includegraphics[width=7.1cm,clip]{6171fig2.eps} \end{figure}$ Figure 2: Evolution of the gas surface density within the inner 10 AU of our simulated disk. The upper solid line is the $r^{-1.5}~\Sigma_{\rm g}$ -profile for a $3\times\mbox{MMSN}$ disk. The lower solid curves, in descending order, are the profiles at 0.1, 0.25, 0.5, 1.0 and 1.5 Myr respectively. The dashed line is the fixed $\Sigma _{\rm g}$ -profile assumed in Paper I.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{6171fig3.eps} \end{figure}$ Figure 3: Semi-major axis evolution of the giant planet in each scenario from the launch time (the top row in Table 2) to the time at which it arrives at 0.1 AU.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{6171fig4.eps} \end{figure}$ Figure 4: Scenario I 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

$\begin{figure} \par\includegraphics[width=12cm,clip]{6171fig5.eps} \end{figure}$ Figure 5: Scenario I at 60 000 years after the start of giant planet migration. The giant has now moved inward to 2.72 AU. Increasing excitation of the orbits of protoplanets captured at resonances is apparent, as is the build-up of matter scattered into external orbits.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{6171fig6.eps} \end{figure}$ Figure 6: Scenario I at 100 000 years after the start of giant planet migration. The giant has now moved inward to 0.70 AU. Five protoplanets are currently crossing the orbit of the giant. The scattered disk has grown and a > $1~{m_\oplus}$ planet is accreting within the compacted interior disk.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{6171fig7.eps} \end{figure}$ Figure 7: Scenario I at 114 000 years after the start of giant planet migration. The giant planet has migrated to 0.1 AU. Most interior mass has been lost after the most massive interior protoplanet impacts the giant. 63% of the original solids disk mass now resides in exterior orbits.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{6171fig8.eps} \end{figure}$ Figure 8: Surface density evolution ( left hand panel) and accretion rates ( right hand panel) for Scenario I. Growing surface density peaks at the 2:1 and 3:2 resonances sweep through the inner system ahead of the giant. Accretion rates increase after $\sim$ 80 000 years within the compacted portion of the disk.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{6171fig9.eps} \end{figure}$ Figure 9: Comparison of the results of Paper I (grey lines and $\times$ symbols) and the results of this paper (black lines and + symbols). Dashed lines and solid lines are the percentage of original disk mass found in the interior and exterior remnants respectively. The ratios of the protoplanet mass fraction in the final exterior disk to that of the original disk, $f_{\rm proto}({\rm final}) \ / f_{\rm proto}({\rm initial})$ , are indicated by the $\times$ and + symbols and are read off the right hand y-axis.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{6171fig10.eps} \end{figure}$ Figure 10: Blow-up of the inner 1 AU of Scenario I, showing eccentricity vs semi-major axis 105 000 years after the start of giant planet migration. Protoplanetary masses are indicated in ${m}_\oplus$ and the locations of the 2:1 and 3:2 resonances are shown with arrows. The giant planet is at 0.45 AU and our hot-Earth candidate is a $1.93~{m}_\oplus$ planet at 0.34 AU with $e \approx 0.03$ . Five lower mass protoplanets are in the process of being scattered into the exterior disk. (Compare with Fig. 6 which shows the situation 5000 years earlier.) As described in Sect. 3.1.1, the hot-Earth candidate is eventually accreted by the giant planet $\sim$ 4000 years later once it has migrated further inward to $\sim$ 0.26 AU.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{6171fig11.eps} \end{figure}$ Figure 11: The total solids mass between 0.75-1.75 AU, before and after the giant planet migration, plotted for each scenario.
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In the text

$\begin{figure} \par\includegraphics[width=12cm,clip]{6171fig12.eps} \end{figure}$ Figure 12: Eccentricities of bodies within 4 AU at the end of Scenario V ( top panel) and after a further 2 Myr of gas-free accretion ( bottom panel). Protoplanets are shown as white circles and are labeled with their mass in ${m}_\oplus$ . Super-planetesimals are indicated by black dots and the grey blob at 0.1 AU is the hot-Jupiter in its post-migration orbit. Gas density at the end of Scenario V is shown as the black curve in the top panel (read off the right-hand axis), the grey curve being the unevolved profile at t = 0.
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In the text

$\begin{figure} \par\includegraphics[width=6.8cm,clip]{6171fig13.eps} \end{figure}$ Figure 13: Composition of the original solids disk in Scenario I ( top panel) compared with the composition of the scattered disk generated through giant planet migration ( bottom panel). The key is explained in the text.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{6171fig1.eps} \end{figure}$	Figure 1: Evolution of the mass of the gas disk. The mass of gas (in Jupiter masses) remaining at the launch point for each of the five migration scenarios is indicated.
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$\begin{figure} \par\includegraphics[width=7.1cm,clip]{6171fig2.eps} \end{figure}$	Figure 2: Evolution of the gas surface density within the inner 10 AU of our simulated disk. The upper solid line is the $r^{-1.5}~\Sigma_{\rm g}$ -profile for a $3\times\mbox{MMSN}$ disk. The lower solid curves, in descending order, are the profiles at 0.1, 0.25, 0.5, 1.0 and 1.5 Myr respectively. The dashed line is the fixed $\Sigma _{\rm g}$ -profile assumed in Paper I.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{6171fig3.eps} \end{figure}$	Figure 3: Semi-major axis evolution of the giant planet in each scenario from the launch time (the top row in Table 2) to the time at which it arrives at 0.1 AU.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{6171fig5.eps} \end{figure}$	Figure 5: Scenario I at 60 000 years after the start of giant planet migration. The giant has now moved inward to 2.72 AU. Increasing excitation of the orbits of protoplanets captured at resonances is apparent, as is the build-up of matter scattered into external orbits.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{6171fig6.eps} \end{figure}$	Figure 6: Scenario I at 100 000 years after the start of giant planet migration. The giant has now moved inward to 0.70 AU. Five protoplanets are currently crossing the orbit of the giant. The scattered disk has grown and a > $1~{m_\oplus}$ planet is accreting within the compacted interior disk.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{6171fig7.eps} \end{figure}$	Figure 7: Scenario I at 114 000 years after the start of giant planet migration. The giant planet has migrated to 0.1 AU. Most interior mass has been lost after the most massive interior protoplanet impacts the giant. 63% of the original solids disk mass now resides in exterior orbits.
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$\begin{figure} \par\includegraphics[width=12cm,clip]{6171fig8.eps} \end{figure}$	Figure 8: Surface density evolution ( left hand panel) and accretion rates ( right hand panel) for Scenario I. Growing surface density peaks at the 2:1 and 3:2 resonances sweep through the inner system ahead of the giant. Accretion rates increase after $\sim$ 80 000 years within the compacted portion of the disk.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{6171fig11.eps} \end{figure}$	Figure 11: The total solids mass between 0.75-1.75 AU, before and after the giant planet migration, plotted for each scenario.
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$\begin{figure} \par\includegraphics[width=6.8cm,clip]{6171fig13.eps} \end{figure}$	Figure 13: Composition of the original solids disk in Scenario I ( top panel) compared with the composition of the scattered disk generated through giant planet migration ( bottom panel). The key is explained in the text.
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