Comparing Accretion Centres Between Rotating and Turbulent Cloud Cores

In this chapter we use the method of Smoothed Particle Hydrodynamics (SPH) to study the number and properties of accretion centres formed when a molecular gas cloud collapses, starting with initial conditions corresponding either to a turbulent or a rigidly rotating sphere. To do so we use a modified version of the SPH code GADGET-2, which is capable to detect when a gas particle becomes an accretion centre, inheriting the mass and momentum of all its closest neighbours. For both types of models (turbulent and uniformly rotating), we also study the effects of considering two different initial mass distributions: a uniform-density and a centrally condensed Plummer profile. We find that the turbulent models are more propense to fragment into a larger number of protostellar objects than the purely rotating clouds. However, in both types of models the average protostellar mass increases with increasing size of the kinetic energy content of the cloud.