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NASA's TESS mission is expected to discover hundreds of M dwarf planets.However, few studies focus on how planets form around low-mass stars. We aim tobetter characterize the formation process of M dwarf planets to fill this gapand aid in the interpretation of TESS results. We use ten sets of N-body planetformation simulations which vary in whether a gas disc is present, initialrange of embryo semi-major axes, and initial solid surface density profile.Each simulation begins with 147 equal-mass embryos around a 0.2 solar mass starand runs for 100 Myr. We find that planets form rapidly, with most collisionsoccurring within the first 1 Myr. The presence of a gas disc reduces the finalnumber of planets relative to a gas-free environment and causes planets tomigrate inward. We find that roughly a quarter of planetary systems experiencetheir final giant impact inside the gas disc, suggesting that some super-Earthsmay be able to reaccrete an extended gaseous envelope after their final giantimpact, though these may be affected by additional process such asphotoevaporation. In addition, we find that the final distribution of planetsdoes not retain a memory of the slope of the initial surface density profile,regardless of whether or not a gas disc is present. Thus, our results suggestthat present-day observations are unlikely to provide sufficient information toaccurately reverse-engineer the initial distribution of solids.

Rapid Formation of Super-Earths Around Low-Mass Stars