in real ellipticals, with the exception of $\epsilon_b$ in model D (see Table 2), which would correspond - if taken at face value - to an E8 galaxy. These result could be just due to the procedure adopted to measure the ellipticity (see Section \[secic\]), however we find interesting that dMOND gravity could be able to produce some system that would be unstable in Newtonian gravity. We remark that a similar result, in the different context of disk stability in MOND, has been obtained by Brada & Milgrom (1999).

In order to describe the radial mass distribution of the final virialized systems, we fitted their angle-averaged density profiles with the $\gamma$-model (\[eqgamma\]) over the radial range $0.06\,\lsim\, r/\rhalf\,\lsim\, 10$. The best-fit $\gamma$ and $\rc$ for the final distribution of each simulation are reported in Table 2 together with their $1\sigma$ uncertainties (calculated from $\Delta
\chi^2=2.30$ contours in the space $\gamma-\rc$). As also apparent from Fig. \[fig3d\] (bottom), the Newtonian collapse produced the system with the steepest inner profile ($\gamma\sim1.7$), the dMOND end-product has inner logarithmic slope close to zero, while MOND collapses led to intermediate cases, with $\gamma$ ranging from $\sim
1.2$ ($\kappa=1$) to $\sim1.5$ ($\kappa=4$). We also note that 