A Fragmentation-Coalescence Model for the Initial Stellar Mass Function: Preliminary Results
A Fragmentation-Coalescence Model for the Initial Stellar Mass Function: Preliminary Results
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初始恒星质量函数的破碎聚结模型：初步结果
DOI：
10.1086/163396
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发表时间：
1985
期刊：
影响因子：
--
通讯作者：
H. Saio
中科院分区：
文献类型：
--
作者：
Y. Yoshii;H. Saio
初始恒星质量函数(IMF)是根据气体云碎裂和碎片间的合并的影响而得出的；Silk(1977)的设想采用了碎裂的设想。如果母星云的半径低于某个临界值，则原恒星产生的热量足以提高气体温度，从而显著提高Jeans质量。然后，在未凝结的气体在恒星形成过程中耗尽之前，国际货币基金组织就会从这个过程中产生。恒星的最大质量是由当地的牛仔长度应该小于先前存在的原恒星之间的平均间隔的约束决定的。参考文献41篇。
The initial stellar mass function (IMF) is derived in light of both the effects of gas cloud fragmentation and coalescence among the fragments; Silk's (1977) scenario in the one adopted for the fragmentation. If the radius of the parent cloud is below some critical value, the heating due to protostars is sufficient to raise the gas temperature, and hence the Jeans mass, considerably. The IMF then arises from this process before the uncondensed gas is used up in the formation of stars. The maximum mass of stars is determined by the constraint that the local Jean length should be smaller than the mean separation among preexisting protostars. 41 references.