标题： 簇中磁云的模拟 显示英文标题

标题： Simulations of the IMF in Clusters

摘要： 我们回顾计算方法以理解星团形成过程中初始质量函数（IMF）的起源。 我们考察湍流、引力和吸积、状态方程以及磁场在产生核心质量分布——核心质量函数（CMF）中的作用。 观测表明，CMF的形态与IMF相似。 我们关注反馈过程，如恒星动力学、辐射和外流可以减少吸积质量，从而产生IMF。 数值工作表明，丝状吸积可能在IMF的起源中起关键作用。 显示英文摘要

摘要： 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.