In the following plots we report plots of i vs. a for the three simulations involving simulated and real members of Adeona.   For the first simulation, of particolar interest are the particles at ~2.7 AU captured into the 8/3 resonance and the two test particles close to the 11/4 resonance that experienced da of ~0.05AU.   Particles in  the second simulation were not significantly spread by close encounters with massive asteroids, and chaotic diffusion was the most effective mechanism of dynamical evolution (see particles in the 5-1-2 and 7-4-2 three-body resonance).
 
 

The results of the Yarkovsky simulation are of most interest:  particles in the g-2g₆+g₆ secular resonance at ~2.722 AU (not shown) do not experience significant changes in i.  The family is bounded by the 8/3 resonance at a~2.71 AU, and is significantly spread by the 11/4.   There are no powerful resonances at the other edge of the family, so the fact we we don't see members of Adeona with a < 2.6 AU may indicate a relatively young age for this family.

Gefion is the family for which the probabillity of close encounters with 1 Ceres is highest in the main belt.   Still, the distribution in a is not significantly altered for real members, while synthetic particles experienced a change in sigma_a of ~30%.   Also, 54% of the test particles at the end of the simulation where displaced by more than 0.001 AU, and 4 particles were displaced by more than 0.005 AU.  We believe that close encounters can have played an important role in modeling the shape of the distribution in proper elements of the largest members of this family.
 
 

About the Yarkovsky simulation,  we are again able to reproduce the distribution in a but not that in i, which is probably due to the conservative value of our choice of initial velocity at infinity.
 
 

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