Adeona is bounded by the 8/3 mean motion resonance with Jupiter, and is crossed by the 11/4.  In the first plot we report the results of the integration of 66 members of this family, the evolution is dominated by chaotic  diffusion (one of the particle is captured by the 8/3 resonance), but there are cases in which the gravitational scattering from large asteroids is significant (see the test particle at a =2.64 AU, e=0.1648, which experiences a change in a of almost 0.005 AU, and the test particle at a=2.652, e=0.157, which, after leaving the 11/4 resonance is scattered by ~0.007AU).  Also, close encounters injected (and expelled) four particles into the 11/4 resonance.
 
 
 

The second plot reports results for the synthetic distribution; the distribution was centered on 145 Adeona, which contains 53% of the mass of the family: as for the case of real members, apart for isolated cases, the dynamical evolution is dominated by chaotic diffusion.   Note that the family is not able to spread across the 11/4 resonance.    Finally, in the third plot, we report the results of the Yarkovksy integrations.  Black dots represents members of the family identified by David Nesvorny using the HCM method with a cutoff of 80 m/s on the database of 1)  66,089 analytically computed (Milani and Knezevic), and 2)  31.502 numerically computed proper elements (Knezevic and Milani). The particles can actually reproduce the distribution in a (note the boundary at the 8/3 resonance with Jupiter), but not the distribution in e (did we choose a too conservative value for the velocity at infinity of the synthetic family?).    Particles that drift beyond ~2.75 AU interact with the g-2g₆+g5 secular resonance (the yellow line in the figure represents the center of the resonance computed for i = 11.6^o  by David Nesvorny) and experience a substantial change in e but not in i (see next section).

Gefion is the family which is most affected by close encounters with Ceres in the entire asteroid belt, and indeed, close encounters are able to change the dispersion in a of the synthetic family by 30% of the original value.   Still, the evolution is dominated by the Yarkovsky effect, which is able to reproduce the dispersion in a of the current members of the family (but again our choice of velocity at infinity was too conservative , and we are not able to reproduce the dispersion in e).   In the Yarkovsky simulation two particles entered the 8/3 mean motion resonance with Jupiter at ~2.72 AU.     Particles at a~2.818 entered the 5/2 resonance and had their eccentricity considerably increased: this seems to agree with the distribution of Gefion members found by using Nesvorny's program and a cutoff of v=80 m/s.  Also, the larger dispersion in e at a~2.75 is most probably due to the 13/5 mean motion and 3-1-1 three body resonances.
 
 
 

  NOT YET AVAILABLE.