An evolutionary scenario for primeval stellar populations
An evolutionary scenario for primeval stellar populations
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原始恒星种群的演化情景
DOI：
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发表时间：
1993
期刊：
影响因子：
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通讯作者：
V. Castellani
中科院分区：
文献类型：
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作者：
S. Cassisi;V. Castellani
我们给出了一个恒星结构的演化计算网格，初始重元素量Z = 10 −10，初始He丰度Y = 0.23。恒星质量范围为0.7 ≤ M ≤ 15 M ○。已经调查，从最初的ZAMS结构的演变，直到他闪光，或更大的质量，到最后冷却的C-O简并核心或C点火。对于Z = 10 −6和Z = 10 −4，给出了并行计算，允许研究当金属丰度从正常的星族II组成降低到预期的重元素宇宙学丰度时恒星结构的演化行为
We present a grid of evolutionary computations of stellar structures with an original amount of heavy elements Z = 10 −10 and for an original He abundance Y = 0.23. The range of stellar masses 0.7 ≤ M ≤ 15 M ○. has been investigated, following the evolution from the initial ZAMS structures till the He flash or, for larger masses, up to the final cooling of the C-O degenerate cores or up to the C ignition. Parallel computations are presented for Z = 10 −6 and Z = 10 −4 , allowing the investigation of the evolutionary behavior of stellar structures when lowering the metallicity from a normal Population II composition down to the expected cosmological abundance of heavy elements