Prestellar Cores in Turbulent Clouds: Numerical Modeling and Evolution to Collapse

Abstract A fundamental issue in star formation is understanding the precise mechanisms leading to the formation of prestellar cores and their subsequent gravitationally unstable evolution. To address this question, we carefully construct a suite of turbulent, self-gravitating numerical simulations, and analyze the development and collapse of individual prestellar cores. We show that the numerical requirements for resolving the sonic scale and internal structure of anticipated cores are essentially the same in self-gravitating clouds, calling for the number of cells per dimension to increase quadratically with the cloud’s Mach number. In our simulations, we follow the evolution of individual cores by tracking the region around each gravitational potential minimum over time. Evolution in nascent cores is toward increasing density and decreasing turbulence, and there is a wide range of critical density for initiating collapse. At a given spatial scale, the turbulence level also varies widely and tends to be correlated with density. By directly measuring the radial forces acting within cores, we identify a distinct transition to a state of gravitational runaway. We use our new theory for turbulent equilibrium spheres to predict the onset of each core’s collapse. Instability is expected when the critical radius becomes smaller than the tidal radius; we find good agreement with the simulations. Interestingly, the imbalance between gravity and opposing forces is only ∼20% during core collapse, meaning that this is a quasi-equilibrium rather than a freefall process. For most of their evolution, cores exhibit both subsonic contraction and transonic turbulence inherited from core-building flows; supersonic radial velocities accelerated by gravity only appear near the end of the collapse.