Simulations of the IMF in Clusters
arXiv:1012.1874 · doi:10.1017/S1743921311000317
Abstract
We review computational approaches to understanding the origin of the Initial Mass Function (IMF) during the formation of star clusters. We examine the role of turbulence, gravity and accretion, equations of state, and magnetic fields in producing the distribution of core masses - the Core Mass Function (CMF). Observations show that the CMF is similar in form to the IMF. We focus on feedback processes such as stellar dynamics, radiation, and outflows can reduce the accreted mass to give rise to the IMF. Numerical work suggests that filamentary accretion may play a key role in the origin of the IMF.
8 pages, 1 (4 part) figure, refereed conference proceedings - invited review, to appear in Proceedings of IAU Symposium 270, 2010 "Computational Star Formation", J. Alves, B.G. Elmegreen, J. Miquel, & V. Trimble (eds.)
References in corpus (20)
- Theory of Star Formation
- Analytical theory for the initial mass function: CO clumps and prestellar cores
- Probing the evolution of molecular cloud structure: From quiescence to birth
- Modeling Collapse and Accretion in Turbulent Gas Clouds: Implementation and Comparison of Sink Particles in AMR and SPH
- Radiation-Hydrodynamic Simulations of Collapse and Fragmentation in Massive Protostellar Cores
- Outflow Feedback Regulated Massive Star Formation in Parsec-Scale Cluster Forming Clumps
- The Importance of Radiative Feedback for the Stellar Initial Mass Function
- Magnetic Braking and Protostellar Disk Formation: The Ideal MHD Limit
- H II regions: Witnesses to massive star formation
- Magnetically Regulated Star Formation in 3D: The Case of Taurus Molecular Cloud Complex
- Protostellar collapse: radiative and magnetic feedbacks on small scale fragmentation
- The seeds of star formation in the filamentary infrared-dark cloud G011.11-0.12
- Inefficient star formation: The combined effects of magnetic fields and radiative feedback
- Radiation Magnetohydrodynamics Simulation of Proto-Stellar Collapse: Two-Component Molecular Outflow
- Large Area Mapping at 850 Microns. V. Analysis of the Clump Distribution in the Orion A South Molecular Cloud
- Supersonic turbulence, filamentary accretion,and the rapid assembly of massive stars and disks
- The Effect of the Interstellar Model on Star Formation Properties in Galactic Disks
- Can Protostellar Jets Drive Supersonic Turbulence in Molecular Clouds?
- Shock generated vorticity in the interstellar medium and the origin of the stellar initial mass function
- Insights from Simulations of Star Formation