All Figures

$\begin{figure} \par\includegraphics[width=8cm,clip]{9865fig1.eps}\end{figure}$ Figure 1: Strength impact. The dashed line represents the $Q_{\rm S}$ law used in our simulations while the $Q_{\rm D}$ law from Benz & Asphaug (1999) for icy bodies at 3 km s^-1 is plotted as a solid line.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{9865fig2.eps}\end{figure}$ Figure 2: Normalized distribution of Plutinos obtained from the dynamical evolution of 197 Plutino candidates extracted from the Minor Planet Center database with semimajor axes between 39 and 40 AU in the planes (a, e) a) and (a, i) b). The color scale depicts the expected density of Plutinos. Blue colors indicate where the Plutinos are statistically most likely to spend their time.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{9865fig3.eps}\end{figure}$ Figure 3: Initial populations of the model.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{9865fig4.eps}\end{figure}$ Figure 4: Our estimates of the Plutino cumulative size distribution after 4.5 Gyr of evolution obtained from the different initial populations proposed in Sect. 4.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{9865fig5.eps}\end{figure}$ Figure 5: Mean collisional lifetimes of Plutinos obtained using the different initial populations defined in Sect. 4. The horizontal short-dashed line represents the age of the Solar System.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{9865fig6.eps}\end{figure}$ Figure 6: Ejection rate of fragments from the 3:2 mean motion resonance with Neptune with diameters greater than 1 km per Myr obtained from the different initial populations defined in Sect. 4.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9865fig7.eps}\end{figure}$ Figure 7: Representative values of semimajor axis, eccentricity and inclination for the fragments ejected from the 3:2 mean motion resonance with Neptune.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=9cm,clip]{9865fig8.eps}\end{figure}$ Figure 8: Distribution of $D \geq$ 1 km Plutino fragments with respect to semimajor axis a, eccentricity e and inclination i. Time evolution from an initial cold population.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{9865fig1.eps}\end{figure}$	Figure 1: Strength impact. The dashed line represents the $Q_{\rm S}$ law used in our simulations while the $Q_{\rm D}$ law from Benz & Asphaug (1999) for icy bodies at 3 km s^-1 is plotted as a solid line.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8.3cm,clip]{9865fig2.eps}\end{figure}$	Figure 2: Normalized distribution of Plutinos obtained from the dynamical evolution of 197 Plutino candidates extracted from the Minor Planet Center database with semimajor axes between 39 and 40 AU in the planes (a, e) a) and (a, i) b). The color scale depicts the expected density of Plutinos. Blue colors indicate where the Plutinos are statistically most likely to spend their time.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{9865fig3.eps}\end{figure}$	Figure 3: Initial populations of the model.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{9865fig4.eps}\end{figure}$	Figure 4: Our estimates of the Plutino cumulative size distribution after 4.5 Gyr of evolution obtained from the different initial populations proposed in Sect. 4.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{9865fig5.eps}\end{figure}$	Figure 5: Mean collisional lifetimes of Plutinos obtained using the different initial populations defined in Sect. 4. The horizontal short-dashed line represents the age of the Solar System.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{9865fig6.eps}\end{figure}$	Figure 6: Ejection rate of fragments from the 3:2 mean motion resonance with Neptune with diameters greater than 1 km per Myr obtained from the different initial populations defined in Sect. 4.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=8cm,clip]{9865fig7.eps}\end{figure}$	Figure 7: Representative values of semimajor axis, eccentricity and inclination for the fragments ejected from the 3:2 mean motion resonance with Neptune.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=9cm,clip]{9865fig8.eps}\end{figure}$	Figure 8: Distribution of $D \geq$ 1 km Plutino fragments with respect to semimajor axis a, eccentricity e and inclination i. Time evolution from an initial cold population.
Open with DEXTER