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Earth-sized planets were observed in close-in orbits around M dwarfs. Whilemore and more planets are expected to be uncovered around M dwarfs, theories oftheir formation and dynamical evolution are still in their infancy. Weinvestigate the giant impact growth of protoplanets, which includes strongscattering around low-mass stars. The aim is to clarify whether strongscattering around low-mass stars affects the orbital and mass distributions ofthe planets. We perform $N$-body simulation of protoplanets by systematicallysurveying the parameter space of the stellar mass and surface density ofprotoplanets. We find that protoplanets are often ejected after twice or threetimes close-scattering around late M dwarfs. The ejection sets the upper limitof the largest planet mass. Adopting the surface density scaling linearly withthe stellar mass, we find that as the stellar mass decreases less massiveplanets are formed in orbits with higher eccentricities and inclinations. Underthis scaling, we also find that a few close-in protoplanets are generallyejected. The ejection of protoplanets plays an important role in the massdistribution of super-Earths around late M dwarfs. The mass relation ofobserved close-in super-Earths and their central star mass is well reproducedby ejection.

Ejection of close-in super-Earths around low-mass stars in the giant impact stage