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Simulations of the IMF in Clusters

Published online by Cambridge University Press:  27 April 2011

Ralph E. Pudritz
Ralph E. Pudritz*
Affiliation:
Origins Institute, McMaster University, ABB 241, Hamilton, Ontario L8S 4M1, Canada email: pudritz@mcmaster.ca
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Abstract

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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

initial mass functionturbulenceaccretionfilamentsmagnetic fieldsfeedback
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S270: Computational Star Formation , May 2010 , pp. 151 - 158
Copyright
Copyright © International Astronomical Union 2011

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