Simulations of the IMF in Clusters

TL;DR

This paper reviews computational models of star cluster formation, emphasizing how turbulence, gravity, magnetic fields, and feedback processes influence the development of the core mass function and its relation to the initial mass function.

Contribution

It synthesizes current simulation approaches and highlights the significance of filamentary accretion and feedback in shaping the IMF during star formation.

Findings

Core Mass Function resembles the IMF in form

Feedback processes can modify stellar mass accretion

Filamentary accretion is crucial in IMF origin

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.