The birth, evolution and death of star clusters

被引:0
|
作者
Kroupa, P [1 ]
机构
[1] Univ Kiel, Inst Theoret Phys & Astrophys, D-24118 Kiel, Germany
来源
FROM DARKNESS TO LIGHT: ORIGIN AND EVOLUTION OF YOUNG STELLAR CLUSTERS | 2001年 / 243卷
关键词
clusters; dynamics; mass segregation; stellar ejection; stars : binary systems; high-mass; brown dwarfs;
D O I
暂无
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
A dense-enough gas-accumulation evolves, over a few Myr of intensifying star formation, to an embedded cluster. If it contains a sufficient amount of mass, 0 stars form and explosively expel the remaining gas, whereas poorer clusters reduce their embryonic gas content more gradually. The sudden expulsion of gas unbinds mast of a rich cluster, but a significant fraction of it can condense by two-body interactions to become an open cluster despite a star-formation efficiency as low as 30 per cent. Poorer clusters survive their gradual mass loss more easily, but have short, relaxation-limited life-times. Pleiades-like clusters may thus form as nuclei of expanding OB associations, by filling their tidal radii and having large (1-2 pc) core-radii. A 'main-sequence' of clusters is thus established. Ultimately, a cluster dies an explosive death through the ever shortening relaxation time, and leaves a remnant that consists of about 4-10 stars arranged in a highly hierarchical and thus long-lived system. Dynamical mass segregation in very young clusters is extremely rapid, and heats a cluster substantially, which is partially of set by the cooling from the disruption of primordial binaries.
引用
收藏
页码:387 / 398
页数:12
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