All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3238fig1.ps} \end{figure}$ Figure 1: Model CI: snapshots taken every 26 orbits from t=60 to t=320 orbits, which is after the convergence of model CI. The radial slices of the density, temperature and azimuthal velocity are taken in the midplane at the location of the planet. Model CI defines the initial values for all the models that start off with an axisymmetric gap.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3238fig2.ps} \end{figure}$ Figure 2: Model CDI: snapshots taken every 2 orbits from t=164 to t=184 orbits. The radial slices of the density are taken in the midplane at the location of the planet. The surface density is azimuthally averaged.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3238fig3.ps} \end{figure}$ Figure 3: Model CDI: ( upper row) accreted mass $m_{\rm a}$ and accretion rate onto the planet $\dot m_{\rm a}$ over time; ( lower row) evolution of the mass contained in the Roche lobe $m_{\rm Ro}$ and mass change in the Roche lobe $\dot m_{\rm Ro}$ in units of Jupiter masses and orbital periods of the planet.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3238fig4.ps} \end{figure}$ Figure 4: Model CDI: evolution of planet migration rate in terms of migration time. The solid curve is based on the torques excluding the Roche lobe and the solid horizontal line is the time average. In addition we plot the torques based on an exclusion of 1.5 and 0.5 Hill radii (dotted and dashed lines respectively). In this particular model the gap is very clean, such that all three torques mostly coincide.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3238fig5.ps} \end{figure}$ Figure 5: Model CD4I: snapshots taken each orbit from t=71 to t=81 orbits. The radial slices of the density are taken in the midplane at the location of the planet. The surface density is azimuthally averaged. The dotted line indicates the values for model CDI for comparison.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3238fig6.ps} \end{figure}$ Figure 6: Model CD4: snapshot at t=5 orbits after the refinement of the grid. Radial slices of density and temperature are taken in the midplane at the location of the planet, while surface density is the azimuthal average. (solid line = Model CD4; dotted line = Model CD; dashed line = Model CDS).
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3238fig7.ps} \end{figure}$ Figure 7: Model CD: evolution of the planet migration rate in terms of migration time. The solid curve is based on the torques excluding the Roche lobe and the solid horizontal line is the time average. In addition we plot the torques based on an exclusion of 0.5 Hill radii (dotted lines) and 1.5 Hill radii (dashed lines). The horizontal lines refer to the time averaged values.
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In the text

$\begin{figure} \par {\includegraphics[width=17cm]{3238fig8C.ps} }% % \end{figure}$ Figure 8: Model DR4: early stage of gap opening. Temperature in the $r-\theta$ plane of the protoplanetary disk at the azimuthal location of the planet. This snapshot is taken after 12 orbits, thus the gap is not completely empty yet. In this early phase the heating by the accretion onto the planet drives a strong convectional flow in the still optically thick disk material above the planet. Brightness is logarithmic temperature (lighter = warmer) ranging from 38 K to 1060 K and vectors give the logarithmic mass flux. We also plot iso-density lines with labels giving values in g cm^-3. Density ranges from 10¹⁵ g cm^-3 up to $1.3 \times 10^{10}$ g cm^-3. See the online edition for a color version of this plot.
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In the text

$\begin{figure} \par\includegraphics[width=7.2cm,clip]{3238fig9.ps} \end{figure}$ Figure 9: Model DR: snapshot taken after t=121 orbits (solid line). Model DR4: after t=141 orbits (dotted line). Model DN: after t=121 orbits (dashed line). Model DN4: snapshot taken after t=55 orbits (dash dotted line). Radial slices of density and temperature are taken in the midplane at the location of the planet, while surface density is the azimuthal average.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3238fig10.ps} \end{figure}$ Figure 10: Model DR: ( upper row) accreted mass $m_{\rm a}$ and accretion rate $\dot m_{\rm a}$ onto the planet over time; ( lower row) evolution of the mass contained in the Roche lobe $m_{\rm Ro}$ and mass change in the Roche lobe $\dot m_{\rm Ro}$ in units of Jupiter masses and orbital periods of the planet.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3238fig11.ps} \end{figure}$ Figure 11: Model DR: evolution of planet migration rate in terms of migration time. The solid curve is based on the torques excluding the Roche lobe and the solid horizontal line is the time average. In addition we plot the torques based on an exclusion of 0.5 Hill radii (dotted lines) and 1.5 Hill radii (dashed lines), plus the time averaged values.
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In the text

$\begin{figure} \par {\includegraphics[width=8.2cm]{VERSION_COULEUR/fig12.EPS.eps} }\end{figure}$ Figure 12: Model DR: density in the midplane of the protoplanetary disk after 121 orbits. Dark means low, light means high density. The density ranges from $2.4 \times 10^{-13}~{\rm g}~{\rm cm}^{-3}$ to $8.3 \times 10^{-11}~{\rm g}~{\rm cm}^{-3}$ . See the online edition for a color version of this plot.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm]{VERSION_COULEUR/fig13.EPS.eps} \end{figure}$ Figure 13: Model DR: temperature in the midplane of the protoplanetary disk after 121 orbits. Brightness corresponds to the logarithm of temperature. Black indicates 10 K and white 800 K. See the online edition for a color version of this plot.
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In the text

$\begin{figure} \par {\includegraphics[width=6.5cm,clip]{3238fig14.ps} }\end{figure}$ Figure 14: Model DR4: pressure scale height in the midplane of the circumplanetary cloud after 141 orbits. Radial location is given in units of Hill radii.
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In the text

$\begin{figure} \par {\includegraphics[width=17cm]{3238fig15C.ps} }% \par % \end{figure}$ Figure 15: Model DR4: Temperature in the $r-\theta$ plane of the protoplanetary disk at the azimuthal location of the planet after 141 orbits. Brightness is logarithmic temperature (lighter = warmer) between 30 K and 1500 K, contours are equi-density lines (in g cm^-3) and vectors give the logarithmic mass flux. See the online edition for a color version of this plot.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3238fig1.ps} \end{figure}$	Figure 1: Model CI: snapshots taken every 26 orbits from t=60 to t=320 orbits, which is after the convergence of model CI. The radial slices of the density, temperature and azimuthal velocity are taken in the midplane at the location of the planet. Model CI defines the initial values for all the models that start off with an axisymmetric gap.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3238fig2.ps} \end{figure}$	Figure 2: Model CDI: snapshots taken every 2 orbits from t=164 to t=184 orbits. The radial slices of the density are taken in the midplane at the location of the planet. The surface density is azimuthally averaged.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{3238fig3.ps} \end{figure}$	Figure 3: Model CDI: ( upper row) accreted mass $m_{\rm a}$ and accretion rate onto the planet $\dot m_{\rm a}$ over time; ( lower row) evolution of the mass contained in the Roche lobe $m_{\rm Ro}$ and mass change in the Roche lobe $\dot m_{\rm Ro}$ in units of Jupiter masses and orbital periods of the planet.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3238fig5.ps} \end{figure}$	Figure 5: Model CD4I: snapshots taken each orbit from t=71 to t=81 orbits. The radial slices of the density are taken in the midplane at the location of the planet. The surface density is azimuthally averaged. The dotted line indicates the values for model CDI for comparison.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3238fig6.ps} \end{figure}$	Figure 6: Model CD4: snapshot at t=5 orbits after the refinement of the grid. Radial slices of density and temperature are taken in the midplane at the location of the planet, while surface density is the azimuthal average. (solid line = Model CD4; dotted line = Model CD; dashed line = Model CDS).
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3238fig7.ps} \end{figure}$	Figure 7: Model CD: evolution of the planet migration rate in terms of migration time. The solid curve is based on the torques excluding the Roche lobe and the solid horizontal line is the time average. In addition we plot the torques based on an exclusion of 0.5 Hill radii (dotted lines) and 1.5 Hill radii (dashed lines). The horizontal lines refer to the time averaged values.
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$\begin{figure} \par\includegraphics[width=7.2cm,clip]{3238fig9.ps} \end{figure}$	Figure 9: Model DR: snapshot taken after t=121 orbits (solid line). Model DR4: after t=141 orbits (dotted line). Model DN: after t=121 orbits (dashed line). Model DN4: snapshot taken after t=55 orbits (dash dotted line). Radial slices of density and temperature are taken in the midplane at the location of the planet, while surface density is the azimuthal average.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{3238fig10.ps} \end{figure}$	Figure 10: Model DR: ( upper row) accreted mass $m_{\rm a}$ and accretion rate $\dot m_{\rm a}$ onto the planet over time; ( lower row) evolution of the mass contained in the Roche lobe $m_{\rm Ro}$ and mass change in the Roche lobe $\dot m_{\rm Ro}$ in units of Jupiter masses and orbital periods of the planet.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3238fig11.ps} \end{figure}$	Figure 11: Model DR: evolution of planet migration rate in terms of migration time. The solid curve is based on the torques excluding the Roche lobe and the solid horizontal line is the time average. In addition we plot the torques based on an exclusion of 0.5 Hill radii (dotted lines) and 1.5 Hill radii (dashed lines), plus the time averaged values.
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$\begin{figure} \par {\includegraphics[width=8.2cm]{VERSION_COULEUR/fig12.EPS.eps} }\end{figure}$	Figure 12: Model DR: density in the midplane of the protoplanetary disk after 121 orbits. Dark means low, light means high density. The density ranges from $2.4 \times 10^{-13}~{\rm g}~{\rm cm}^{-3}$ to $8.3 \times 10^{-11}~{\rm g}~{\rm cm}^{-3}$ . See the online edition for a color version of this plot.
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$\begin{figure} \par\includegraphics[width=8.2cm]{VERSION_COULEUR/fig13.EPS.eps} \end{figure}$	Figure 13: Model DR: temperature in the midplane of the protoplanetary disk after 121 orbits. Brightness corresponds to the logarithm of temperature. Black indicates 10 K and white 800 K. See the online edition for a color version of this plot.
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$\begin{figure} \par {\includegraphics[width=6.5cm,clip]{3238fig14.ps} }\end{figure}$	Figure 14: Model DR4: pressure scale height in the midplane of the circumplanetary cloud after 141 orbits. Radial location is given in units of Hill radii.
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$\begin{figure} \par {\includegraphics[width=17cm]{3238fig15C.ps} }% \par % \end{figure}$	Figure 15: Model DR4: Temperature in the $r-\theta$ plane of the protoplanetary disk at the azimuthal location of the planet after 141 orbits. Brightness is logarithmic temperature (lighter = warmer) between 30 K and 1500 K, contours are equi-density lines (in g cm^-3) and vectors give the logarithmic mass flux. See the online edition for a color version of this plot.
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