Evolution of 0. 7--3. 0 M/sub sun/ stars having -1. 0< or =(Fe/H)< or =0. 0
Evolution of 0. 7--3. 0 M/sub sun/ stars having -1. 0< or =(Fe/H)< or =0. 0
复制标题
0。7--3的演变。
DOI：
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发表时间：
1985
期刊：
影响因子：
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通讯作者：
D. VandenBerg
中科院分区：
文献类型：
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作者：
D. VandenBerg
五个网格的恒星模型的质量范围从0.7到3.0 M/sub - sun/，依次假设金属丰度(Fe/H) = -1.0, -0.76, -0.46, -0.23和0.0。所有的计算都是基于Y = 0.25的氦含量和…为混合长度与压标高度之比= 1.6。在不透明数据和核反应速率方面的最新改进已被纳入计算。此外，模型大气已被用来为恒星内部计算提供边界条件，并将年龄从0.3 × 10/sup 9/到15 × 10/sup 9/年计算的等时线从理论面转置到（M/sub v/, B-V）面。表兄弟V-I和V-R颜色也预测了每个模型序列，这是广泛的表格。
Five grids of stellar models have been calculated for masses ranging from 0.7 to 3.0 M/sub sun/ assuming, in turn, a metal abundance (Fe/H) = -1.0, -0.76, -0.46, -0.23, and 0.0. All of the calculations are based on a value of Y = 0.25 for the helium content and ..cap alpha.. = 1.6 for the ratio of the mixing length to the pressure scale height. The latest improvements in opacity data and nuclear reaction rates have been incorporated into the computations. Moreover, model atmospheres have been used to provide the boundary conditions for the stellar interior calculations as well as to transpose the isochrones, computed for ages from 0.3 x 10/sup 9/ to 15 x 10/sup 9/ yr, from the theoretical to the (M/sub v/, B-V)-plane. Cousins V-I and V-R colors are also predicted for each of the model sequences, which are extensively tabulated.