All Figures

$\begin{figure} \par\includegraphics[angle=-90, width=7.5cm,clip]{6729fig1.eps}\end{figure}$ Figure 1: Comparison between the protoplanet effective radius for planetesimal capture. In solid line, $R^*_{\rm eff}$ is calculated using Eq. (11) and in dashed-dotted line $R_{\rm eff}$ is calculated including the gas drag of the atmosphere. These results were obtained with a full evolutionary numerical simulation. The protoplanetary disc surface density corresponds to a 6 MMSN. The protoplanet is located at 5.2 AU and the radius of incoming planetesimals is 100 km.
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width=7.5cm,clip]{6729fig2.eps}\end{figure}$ Figure 2: Comparison case. We plot the mass evolution of the core (solid line), of the envelope (dash-dotted line) and of the total mass (dashed line) of the protoplanet. The input parameters of this run are the same as those of case J3 of Pollack et al. (1996). This figure should be compared to Fig. 2b of the cited article. See the text for details.
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width=7.5cm,clip]{6729fig3.eps}\end{figure}$ Figure 3: For the same comparison case as in Fig. 2, solid (dashed-dotted) line shows the time evolution of the logarithm of the core (envelope) growth rate.
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In the text

$\begin{figure} \par\includegraphics[angle=-90,width=6.5cm,clip]{6729fig4.eps}\end{figure}$ Figure 4: The impact of the selected model for the growth of the core. The solid line shows the ratio of eccentricities e/e_*, where e is calculated according to Eq. (13) and e_* according to the model adopted by Pollack et al. (1996). The dashed-dotted line plots the ratio of inclinations i/i_*. While in our model i depends on e (i=e/2), in Pollack et al.(1996) i_* remains constant during the entire simulation. For the X axis we selected the Hill radius in order to get rid of the different formation timescales of both simulations.
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width=7.5cm,clip]{6729fig5.eps}\vspace*{4mm} \includegraphics[angle=-90, width=7.5cm,clip]{6729fig6.eps}\end{figure}$ Figure 5: For a 6 MMSN protoplanetary disc, panel a) shows the core (solid line) and envelope (dashed-dotted line) mass evolution of a Jupiter-like forming protoplanet at 5.2 AU, considering that the core grows according to the oligarchic growth regime, with $R^*_{\rm eff}$ calculated with Eq. (11). Panel b) shows the same simulation but including the gas drag effect of the protoplanetary atmosphere in the calculation of $R_{\rm eff}$ . Note that for a clear visualisation the Y axis changes from a linear scale to a logarithmic scale. Panel a) ( b)) is in a linear scale up to $40 \; {M_{\oplus}}$ ( $100 \; {M_{\oplus}}$ ), afterwards the scale is logarithmic. For both runs, planetesimal radius was set equal to 100 km.
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width= 7.2cm,clip]{6729fig7.eps}\end{figure}$ Figure 6: This panel depicts the evolution of the solids surface density for the simulation that includes the atmospheric gas drag (corresponding to Fig. 5b). A core of $\sim$ $10 \; { M_{\oplus}}$ is achieved for $t \sim 6. 5 \; {\rm My}$ , when $\Sigma$ is still very high.
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width= 7.7cm,clip]{6729fig8.eps}\end{figure}$ Figure 7: This figure shows the evolution of the core accretion rate for the simulation that includes atmospheric gas drag. Note that the accretion rate is still an increasing function when the mass of the core reaches 10 ${M_{\oplus }}$ (corresponding to $\sim$ ${\rm 6.5 \; My}$ ; see also Fig. 5b), preventing the rapid accretion of the envelope mass.
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width=7.7cm,clip]{6729fi9.eps}\vspace*{4mm} \includegraphics[angle=-90, width=7.7cm,clip]{6729fi10.eps}\end{figure}$ Figure 8: For a protoplanetary disc of 6 MMSN and planetesimals having a radius of 10 km, upper panel a) shows the evolution of the protoplanet mass (the core mass with the solid line, the envelope mass with the dashed-dotted line) when no atmospheric gas drag is considered. The lower panel b) illustrates the same process but when $R_{\rm eff}$ is calculated including the gas drag force acting on incoming planetesimals. Again, the Y axis is split in two different scales: first we adopt a linear scale and then a logarithmic one. The same range as in Fig. 5 is adopted.
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In the text

$\begin{figure} \par\includegraphics[angle=-90, width=7.5cm,clip]{6729fig2.eps}\end{figure}$	Figure 2: Comparison case. We plot the mass evolution of the core (solid line), of the envelope (dash-dotted line) and of the total mass (dashed line) of the protoplanet. The input parameters of this run are the same as those of case J3 of Pollack et al. (1996). This figure should be compared to Fig. 2b of the cited article. See the text for details.
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$\begin{figure} \par\includegraphics[angle=-90, width=7.5cm,clip]{6729fig3.eps}\end{figure}$	Figure 3: For the same comparison case as in Fig. 2, solid (dashed-dotted) line shows the time evolution of the logarithm of the core (envelope) growth rate.
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$\begin{figure} \par\includegraphics[angle=-90, width= 7.2cm,clip]{6729fig7.eps}\end{figure}$	Figure 6: This panel depicts the evolution of the solids surface density for the simulation that includes the atmospheric gas drag (corresponding to Fig. 5b). A core of $\sim$ $10 \; { M_{\oplus}}$ is achieved for $t \sim 6. 5 \; {\rm My}$ , when $\Sigma$ is still very high.
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$\begin{figure} \par\includegraphics[angle=-90, width= 7.7cm,clip]{6729fig8.eps}\end{figure}$	Figure 7: This figure shows the evolution of the core accretion rate for the simulation that includes atmospheric gas drag. Note that the accretion rate is still an increasing function when the mass of the core reaches 10 ${M_{\oplus }}$ (corresponding to $\sim$ ${\rm 6.5 \; My}$ ; see also Fig. 5b), preventing the rapid accretion of the envelope mass.
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