All Figures

$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f1.ps}\end{figure}$ Figure 1: Size distribution for the low-mass nominal system (see Table 3) at 5 different epochs. Note that the y-axis displays the mass contained in one size bin, which is a correct way of displaying the mass distribution since all size bins are equally spaced in a logarithmic scale. This plot is more "visual" than a more classical ${\rm d}N(R)$ one, since it can be directly interpreted in terms of mass contribution (and mass loss or mass increase) of each size range to the total mass.
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In the text

$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f2.ps}\end{figure}$ Figure 2: Temporal evolution of the system's total mass for different cases.
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In the text

$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f3.ps}\end{figure}$ Figure 3: Temporal evolution of the ratio $M_{\rm dust}/M_{\rm planetesimals}$ for different cases, where $M_{\rm dust}$ is the total mass of all objects smaller than 1 mm and $M_{\rm planetesimals}$ is the mass of all objects bigger than 10 km. The horizontal line gives the initial value corresponding to an academic ${\rm d}N~=~CR^{-3.5}{\rm d}R$ size distribution.
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In the text

$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f4.ps}\end{figure}$ Figure 4: Size distribution at 5 different epochs for the massive-disc case, where the total mass of the system is chosen in order to match the planetesimal mass estimates deduced from FEB mechanism analysis (see Sect. 2.2).
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In the text

$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f5.ps}\end{figure}$ Figure 5: Temporal evolution of the system's total mass for the massive disc case.
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In the text

$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f6.ps}\end{figure}$ Figure 6: Final distribution (at t=10⁷ years) for different levels of the disc's dynamical excitation.
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In the text

$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f7.ps}\end{figure}$ Figure 7: Final distribution (at t=10⁷ years) for different values of $R_{\rm pr}$ .
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In the text

$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f8.ps}\end{figure}$ Figure 8: Final mass distribution (at t=10⁷ years) for different Q_* prescriptions.
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In the text

$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f9.ps}\end{figure}$ Figure 9: Final mass distribution (at t=10⁷ years) for different values of the free parameters of our bimodal power law: i.e. the ratio of their slopes q₁/q₂ and the position of the slope changing size $R_{\rm s}$ with respect to the size $R_{\rm i}$ of the impacted body.
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In the text

$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f10.ps}\end{figure}$ Figure 10: Final mass distribution (at t=10⁷ years) for different values of the excavation coefficient $\alpha$ .
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In the text

$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f11.ps}\end{figure}$ Figure 11: Final mass distribution (at t=10⁷ years) for an academic case with a very efficient removal of small particles by hypothetic collisions in the r>10 AU region (see text for details).
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In the text

$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f12.ps}\end{figure}$ Figure 12: Typical lifetime, as a function of its size, of a dust particle in the inner disc before destruction by collision (steady state regime of the nominal case).
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In the text

$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f2.ps}\end{figure}$	Figure 2: Temporal evolution of the system's total mass for different cases.
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$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f3.ps}\end{figure}$	Figure 3: Temporal evolution of the ratio $M_{\rm dust}/M_{\rm planetesimals}$ for different cases, where $M_{\rm dust}$ is the total mass of all objects smaller than 1 mm and $M_{\rm planetesimals}$ is the mass of all objects bigger than 10 km. The horizontal line gives the initial value corresponding to an academic ${\rm d}N~=~CR^{-3.5}{\rm d}R$ size distribution.
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$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f4.ps}\end{figure}$	Figure 4: Size distribution at 5 different epochs for the massive-disc case, where the total mass of the system is chosen in order to match the planetesimal mass estimates deduced from FEB mechanism analysis (see Sect. 2.2).
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$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f5.ps}\end{figure}$	Figure 5: Temporal evolution of the system's total mass for the massive disc case.
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$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f6.ps}\end{figure}$	Figure 6: Final distribution (at t=10⁷ years) for different levels of the disc's dynamical excitation.
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$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f7.ps}\end{figure}$	Figure 7: Final distribution (at t=10⁷ years) for different values of $R_{\rm pr}$ .
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$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f8.ps}\end{figure}$	Figure 8: Final mass distribution (at t=10⁷ years) for different Q_* prescriptions.
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$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f9.ps}\end{figure}$	Figure 9: Final mass distribution (at t=10⁷ years) for different values of the free parameters of our bimodal power law: i.e. the ratio of their slopes q₁/q₂ and the position of the slope changing size $R_{\rm s}$ with respect to the size $R_{\rm i}$ of the impacted body.
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$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f10.ps}\end{figure}$	Figure 10: Final mass distribution (at t=10⁷ years) for different values of the excavation coefficient $\alpha$ .
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$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f11.ps}\end{figure}$	Figure 11: Final mass distribution (at t=10⁷ years) for an academic case with a very efficient removal of small particles by hypothetic collisions in the r>10 AU region (see text for details).
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$\begin{figure} \par\includegraphics[angle=0,origin=br,width=8.8cm]{ms3759f12.ps}\end{figure}$	Figure 12: Typical lifetime, as a function of its size, of a dust particle in the inner disc before destruction by collision (steady state regime of the nominal case).
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