but is still oscillating at very late times because of the oscillations of $K$, while $W$ is constant as expected. As we show in Section \[secphsp\], these oscillations are related to a peculiar behavior of the system in phase space. Finally, simulation M1 (central column) represents an intermediate case between models N and D: the system starts as dMOND, but soon its core becomes concentrated enough to enter the Newtonian regime. After the initial phases of the collapse, Newtonian gravity acts effectively in damping the oscillations of the virial ratio. Overall, it is apparent how the system is in a “mixed” state, neither Newtonian ($K+W$ is not conserved) nor dMOND ($W$ is not constant).

Properties of the collapse end-products
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### Spatial and projected density profiles

We found that all the simulated systems, once virialized, are not spherically symmetric. However, while the dMOND collapse end-product is triaxial ($c/a\sim0.2$, $b/a\sim0.4$), MOND and Newtonian end-products are oblate ($c/a \sim c/b \sim 0.5$). The ellipticity $\epsilon$ of the projected density distributions (measured for each of the principal projections) is found in the range $0.5-0.8$ in D, and $0 - 0.5$ in M1, M2, M4 and N. These values are consistent with those observed 