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Planets between 1-4 Earth radii with orbital periods <100 days are strikinglycommon. The migration model proposes that super-Earths migrate inwards and pileup at the disk inner edge in chains of mean motion resonances. After gas diskdispersal, simulations show that super-Earth's gravitational interactions cannaturally break their resonant configuration leading to a late phase of giantimpacts. The instability phase is key to matching the orbital spacing ofobserved systems. Yet, most previous simulations have modelled collisions asperfect accretion events, ignoring fragmentation. In this work, we investigatethe impact of imperfect accretion on the breaking the chains scenario. Weperformed N-body simulations starting from distributions of planetary embryosand modelling the effects of pebble accretion and migration in the gas disk.Our simulations also follow the long-term dynamical evolution of super-Earthsafter the gas disk dissipation. We compared the results of simulations wherecollisions are treated as perfect merging events with those where imperfectaccretion and fragmentation are allowed. We concluded that the perfectaccretion is a suitable approximation in this regime, from a dynamical point ofview. Although fragmentation events are common, only ~10% of the system mass isfragmented during a typical "late instability phase", with fragments beingmostly reacreted by surviving planets. This limited total mass in fragmentsproved to be insufficient to alter qualitatively the final system dynamicalconfiguration -- e.g. promote strong dynamical friction or residual migration-- compared to simulations where fragmentation is neglected.

The "Breaking The Chains" migration model for super-Earths formation: the effect of collisional fragmentation