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$\begin{figure} \par\includegraphics[width=5.8cm,clip]{3355f1a.eps}\hspace*{4mm} \includegraphics[width=5.8cm,clip]{3355f1b.eps} \end{figure}$ Figure 1: Location in proper element space (a-e, a); a-i, b)) of the 5112 asteroids (small dots) members of the Vesta family (Mothè-Diniz et al. 2005). The black triangle shows the location of 4 Vesta itself, while the ellipse displays the 600 m/s level of maximum ejection velocity. The other dots show the locations of the 22 V-type asteroids that are not members of the family.
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In the text

$\begin{figure} \par\includegraphics[width=8.5cm,clip]{3355f2.eps} \end{figure}$ Figure 2: Location of the nonlinear secular resonances in the 4 Vesta region, computed for the inclination of 4 Vesta ( $i = 6.357^{\circ }$ ), in the osculating a-e plane, determined with the Spectral Analysis Method (SAM hereafter, Michtchenko et al. 2002). In blue we show the resonances of perihelia, in green those of nodes, and in magenta those of both perihelia and nodes. For reference we also show the locations in proper element space of 4 Vesta (triangle) the Vesta family members (small dots) and of the V-type asteroids outside the family (full dots). The thick lines display the location of the z₂ (in blue) and ${\gamma }_2$ (in magenta) resonances. For the identification of the other nonlinear secular resonances see Table 1).
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In the text

$\begin{figure} \includegraphics[width=8.5cm,clip]{3355f3.eps} \end{figure}$ Figure 3: The plot shows the location of the z₂ ( 2(g-g₆)+s-s₆) secular resonance (black asterisks), of the ${\gamma }_2$ ( 2g-2g₆+g₅-g₄) (red circles), and of the 3J+1S-1A, 8J-3S-2A, and 5J-4S-1A three-body resonances (vertical lines), as found by plotting the resonant arguments of the test particles. The black full circle displays the actual position of 956 Elisa, and small dots show all the initial conditions used. The 3J+1S-1A resonance lies in the band from 2.29880 to 2.29910 AU (as compared with the analytical result of Nesvorny & Morbidelli 1998, of 2.2994 AU).
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{3355f4a.eps}\hspace*{4mm} \includegraphics[width=5.8cm,clip]{3355f4b.eps} \end{figure}$ Figure 4: The averaged a-e and a-i evolution of two 100 m clones of 956 Elisa. In black we show the evolution of the prograde clone, in red of the retrograde one. The arrows show the two directions of evolution in a, starting from 956 Elisa (black full dot). Small dots show the orbital location of members of the Vesta dynamical family. The magenta line in Fig. 4a gives the location of the z₂ secular resonance, computed for the inclination of Vesta (see Fig. 2) and is given for reference. Note how the clone of Elisa crosses the three-body resonances (3J+1S-1A and 5J-4S-1A, where hereafter J stands for Jupiter, S for Saturn, M for Mars, U for Uranus, and A for asteroid), while remaining inside the z₂ resonance (its path in the a-e plane is inclined, while it should be a horizontal line if the particle were freely drifting due to Yarkovsky effect). The clone leaves the resonance only when interacting with the 1J-1S+1M-2A four-body resonance. It then freely drifts due to the Yarkovsky effect until it reaches the 7J-2A resonance where it is temporary captured.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{3355f5.eps} \end{figure}$ Figure 5: Evolution of the osculating semimajor when the 100 m clone of 956 Elisa crossed the 3J+1S-1A mean motion resonance.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=5.8cm,clip]{3355f6a.eps} \hspace*{4mm} \includegraphics[width=5.8cm,clip]{3355f6b.eps} } \end{figure}$ Figure 6: The argument of the z₂ resonance for the two 100 m Elisa clones evolving under the Yarkovsky effect. a) shows the resonant argument for the clone evolving towards larger a, when passing through the 8J-3S-2A mean-motion resonance. b) shows the argument of the clone evolving towards smaller a, when crossing the 1J-1S+1M-2A four-body resonance (in this case the clone leaves the z₂ secular resonance). The resonant angles have been processed through a digital filter in order to remove all frequencies with periods smaller than 300 000 yr.
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In the text

$\begin{figure} \par\mbox{\includegraphics[width=5.8cm,clip]{3355f7a.eps} \hspace*{4mm} \includegraphics[width=5.8cm,clip]{3355f7b.eps} } \end{figure}$ Figure 7: The proper a-e and a-i evolution of two 100 m clones of 809 Lundia. In black we show the averaged elements of the prograde clone and in red those of the retrograde one. The arrows show the directions of propagation. In the region between the 7J-2A and the 5J-4S-1A the clone never leaves the z₂ secular resonance.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{3355f8.eps} \end{figure}$ Figure 8: Averaged a-e evolution of a 4000 m clone of Elisa. The particle is temporarily captured into the 3J+1S-1A three-body resonance, passes through the 8J-3S-2A resonance, and is finally captured into the ${\gamma }_2$ secular resonance. The black arrow displays the direction of propagation.
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In the text

$\begin{figure} \par\mbox{ \includegraphics[width=5.8cm,clip]{3355f9a.eps} \hspace*{4mm} \includegraphics[width=5.8cm,clip]{3355f9b.eps} } \end{figure}$ Figure 9: Averaged a-e a), and a-i b) evolutions of a 8000 m radius asteroid near the 5J-4S-1A three-body resonance under the effect of the Yarkovsky force. The black arrows show the directions of propagation. The full dot shows the location (in proper element space) of 956 Elisa, while the small dots identify Vesta-family members. Only asteroids with R > 8 km can be captured in the three-body resonance and remain inside it for time long enough to reach the transition region with the z₂ resonance. Once there, the particle was captured in the z₂ resonance, and drifted until reaching values of a, e, and i comparable to those of 956 Elisa.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{3355f10.eps} \end{figure}$ Figure 10: Neighbors of 809 Lundia and 956 Elisa obtained with hierarchical clustering method for an absolute magnitude of 14, and a cutoff velocity of 130 m/s (Zappalà et al. 1990). The asteroids currently in the z₂ resonance are indicated by full dots, while the non-resonant ones are shown by empty dots. The diagonal line displays the location of the z₂ secular resonance, computed for the inclination of 4 Vesta, in osculating a-e space. Small dots show the orbits of family members. Note how 4278 Harvey could have been found by using this method.
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In the text

$\begin{figure} \par\includegraphics[width=5.8cm,clip]{3355f1a.eps}\hspace*{4mm} \includegraphics[width=5.8cm,clip]{3355f1b.eps} \end{figure}$	Figure 1: Location in proper element space (a-e, a); a-i, b)) of the 5112 asteroids (small dots) members of the Vesta family (Mothè-Diniz et al. 2005). The black triangle shows the location of 4 Vesta itself, while the ellipse displays the 600 m/s level of maximum ejection velocity. The other dots show the locations of the 22 V-type asteroids that are not members of the family.
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$\begin{figure} \par\includegraphics[width=7cm,clip]{3355f5.eps} \end{figure}$	Figure 5: Evolution of the osculating semimajor when the 100 m clone of 956 Elisa crossed the 3J+1S-1A mean motion resonance.
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$\begin{figure} \par\mbox{\includegraphics[width=5.8cm,clip]{3355f7a.eps} \hspace*{4mm} \includegraphics[width=5.8cm,clip]{3355f7b.eps} } \end{figure}$	Figure 7: The proper a-e and a-i evolution of two 100 m clones of 809 Lundia. In black we show the averaged elements of the prograde clone and in red those of the retrograde one. The arrows show the directions of propagation. In the region between the 7J-2A and the 5J-4S-1A the clone never leaves the z₂ secular resonance.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{3355f8.eps} \end{figure}$	Figure 8: Averaged a-e evolution of a 4000 m clone of Elisa. The particle is temporarily captured into the 3J+1S-1A three-body resonance, passes through the 8J-3S-2A resonance, and is finally captured into the ${\gamma }_2$ secular resonance. The black arrow displays the direction of propagation.
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