On the mass function of star clusters
On the mass function of star clusters
复制标题
星团的质量函数
DOI：
10.1046/j.1365-8711.2002.05848.x
复制
发表时间：
2002
影响因子：
4.8
通讯作者：
C. Boily
中科院分区：
文献类型：
--
作者：
P. Kroupa;C. Boily
总共形成10 3 <N <10 5恒星的星团（II型星团）由于O星的光电离通量而在动力学时间内失去气体。稀疏（I型）的集群摆脱他们的残余气体在一个时间尺度更长或相当于标称的交叉时间，从而演变近似螺旋。这也是真实的大规模嵌入式集群（III型）的速度色散大于声速的电离气体。因此，在排出残余气体时，I型和III型星团预计会比II型星团损失更少的恒星成分。我们概述了嵌入式集群（ECMF），这是直接相关的星团形成分子云核心的质量函数的质量函数的转换的效果，“初始”MF的束缚无气体星星集群（ICMF）。由此产生的ICMF，为一个无特色的幂律ECMF，营业额近10 4.5兆焦耳和10 3兆焦耳附近的峰值。这座山峰位于毕宿星团、Praesepe星团和Pleiades星团的初始质量周围。我们还发现，如果星星的形成是通过嵌入的星团来进行的，那么整个银河系星族II恒星球状体都可以产生，这些星团的分布类似于指数为0.9<< 2.6的幂律MF。
Clusters that form in total 10 3 <N <10 5 stars (type II clusters) lose their gas within a dynamical time as a result of the photo-ionising flux from O stars. Sparser (type I) clusters get rid of their residual gas on a timescale longer or comparable to the nominal crossing time and thus evolve approximately adiabatically. This is also true for massive embedded clusters (type III) for which the velocity dispersion is larger than the sound speed of the ionised gas. On expelling their residual gas, type I and III clusters are therefore expected to lose a smaller fraction of their stellar component than type II clusters. We outline the effect this has on the transformation of the mass function of embedded clusters (ECMF), which is directly related to the mass function of star-cluster-forming molecular cloud cores, to the “initial” MF of bound gas-free star clusters (ICMF). The resulting ICMF has, for a featureless power-law ECMF, a turnover near 10 4.5 M⊙ and a peak near 10 3 M⊙. The peak lies around the initial masses of the Hyades, Praesepe and Pleiades clusters. We also find that the entire Galactic population II stellar spheroid can be generated if star formation proceeded via embedded clusters distributed like a power-law MF with exponent 0.9< � < 2.6.
影响因子：
3.2
作者：
V. Mannings;A. Boss;S. Russell
通讯作者：
V. Mannings;A. Boss;S. Russell