Statistical analysis of stellar evolution
Statistical analysis of stellar evolution
复制标题
恒星演化的统计分析
DOI：
10.1214/08-aoas219
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发表时间：
2009
期刊：
影响因子：
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通讯作者：
T. Hippel
中科院分区：
文献类型：
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作者：
D. V. Dyk;S. DeGennaro;N. Stein;W. Jefferys;T. Hippel
颜色星等图 (CMD) 是比较不同光波长（颜色）下恒星星等（光度）的图。新形成恒星的质量、颜色和表面温度之间的高度非线性相关性在被称为主序带的 CMD 中产生了狭长的弯曲点云。衰老的恒星形成新的红巨星和白矮星 CMD 群。控制这种演化的物理过程可以用数学模型来描述，并使用复杂的计算机模型来探索。这些计算旨在预测绘制的星等作为科学兴趣参数的函数，例如恒星年龄、质量和金属丰度。在这里，我们描述了如何使用计算机模型作为贝叶斯分析中复杂似然函数的组成部分，贝叶斯分析需要复杂的计算，纠正场恒星对数据的污染，解释未解决的双星系统引起的复杂性，并旨在比较基于物理的恒星演化计算机模型。
Color-Magnitude Diagrams (CMDs) are plots that compare the magnitudes (luminosities) of stars in different wavelengths of light (colors). High nonlinear correlations among the mass, color, and surface temperature of newly formed stars induce a long narrow curved point cloud in a CMD known as the main sequence. Aging stars form new CMD groups of red giants and white dwarfs. The physical processes that govern this evolution can be described with mathematical models and explored using complex computer models. These calculations are designed to predict the plotted magnitudes as a function of parameters of scientific interest, such as stellar age, mass, and metallicity. Here, we describe how we use the computer models as a component of a complex likelihood function in a Bayesian analysis that requires sophisticated computing, corrects for contamination of the data by field stars, accounts for complications caused by unresolved binary-star systems, and aims to compare competing physics-based computer models of stellar evolution.