Simulations of the IMF in Clusters
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.
Keywords
Cite
@article{arxiv.1012.1874,
title = {Simulations of the IMF in Clusters},
author = {Ralph E. Pudritz},
journal= {arXiv preprint arXiv:1012.1874},
year = {2015}
}
Comments
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.)