Modelling star cluster formation: Gas accretion

The formation of star clusters involves the growth smaller, gas-rich subclusters through accretion gas from giant molecular cloud within which are embedded. two main mechanisms responsible for this dense filaments, and ambient background cloud. We perform simulations both these processes onto using coupled smoothed particle hydrodynamics to model gas, N-body dynamics stars. find that, processes, accreting cluster loses some its original mass while gaining either or filament. amount lost is small compared total cluster. However, in case a medium, net effect can be decrease if it travelling fast enough medium ($> 4$kms$^{-1}$). that filamentary independent density, width, number filaments funneling into always such constantly increasing with time. compare our results idealized prescriptions used larger scale GMC act as an upper limit when describing they represent.