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It is thought that young stellar clusters begin their lives with a highly clumpy stellar distribution. Using an N-Body code we have investigated the evolution of initially fractal clusters and the effects that this has on mass segregation. Our results show that cold, highly fractal clusters collapse and evolve into mass segregated clusters on a short timescale, while smooth initially virialised clusters show mass segregation to a much lesser degree. We suggest that the inclusion of substructure is important for understanding the evolution of young clusters and the origin of mass segregation.
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