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Planet-planet collisions are a common outcome of instability in systems oftransiting planets close to the star, as well as occurring during in-situformation of such planets from embryos. Previous N-body studies of instabilityamongst transiting planets have assumed that collisions result in perfectmerging. Here, we explore the effects of implementing a more realisticcollision prescription on the outcomes of instability and in-situ formation atorbital radii of a few tenths of an au. There is a strong effect on the outcomeof the growth of planetary embryos, so long as the debris thrown off incollisions is rapidly removed from the system (which happens by collisionalprocessing to dust, and then removal by radiation forces) and embryos are small($< 0.1\mathrm{\,M}_\oplus$). If this is the case, then systems form fewerdetectable ($\gtrsim1\mathrm{\,M}_\oplus$) planets than systems evolved underthe assumption of perfect merging in collisions. This provides somecontribution to the "Kepler Dichotomy": the observed over-abundance ofsingle-planet systems. The effects of changing the collision prescription onunstable mature systems of super-Earths are less pronounced. Perfect mergersonly account for a minority of collision outcomes in such systems, but mostcollisions resulting in mass loss are grazing impacts in which only a few percent. of mass is lost. As a result, there is little impact on the final massesand multiplicities of the systems after instability when compared to systemsevolved under the assumption that collisions always result in perfect merging.

The dynamical evolution of transiting planetary systems including a realistic collision prescription