Evolutionary synthesis of stellar populations: a modular tool
Evolutionary synthesis of stellar populations: a modular tool
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DOI：
10.1046/j.1365-8711.1998.01947.x
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发表时间：
1998-07
影响因子：
4.8
通讯作者：
C. Maraston
中科院分区：
文献类型：
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作者：
C. Maraston
提出了一种用于恒星种群演化综合的新工具，它基于三个独立的矩阵，分别给出（1）每个演化阶段的燃料消耗作为恒星质量的函数，（2）这些阶段的典型温度和重力，以及（3）作为重力和温度的函数的颜色和辐射热校正。代码的模块化结构使人们能够轻松评估各种假设和模型成分对合成光谱能量分布的影响，例如恒星演化模型中的不确定性、混合长度、水平分支恒星的温度分布、渐近巨分支质量损失和色温变换。麦哲伦云团中所谓的“AGB相变”用于校准热脉冲渐近巨分支相对合成积分光度的贡献。作为说明性示例，提出了太阳金属丰度（Y = 0.27，Z = 0.02）模型，其年龄范围在 30 Myr 到 15 Gyr 之间，并且提供了初始质量函数斜率的各种选择。将合成的宽带颜色和各个演化阶段的光度贡献与大麦哲伦星云和银河球状星团数据进行比较。在所有这些情况下，都达成了良好的协议。最后，介绍了辐射热和 UBVRK 通带中恒星质光比的演变，其中考虑了恒星残余物的贡献。
A new tool for the evolutionary synthesis of stellar populations is presented, which is based on three independent matrices, giving respectively (1) the fuel consumption during each evolutionary phase as a function of stellar mass, (2) the typical temperatures and gravities during such phases, and (3) the colours and bolometric corrections as functions of gravity and temperature. The modular structure of the code allows one easily to assess the impact on the synthetic spectral energy distribution of the various assumptions and model ingredients, such as, for example, uncertainties in stellar evolutionary models, the mixing length, the temperature distribution of horizontal branch stars, asymptotic giant branch mass loss, and colour–temperature transformations. The so-called ‘AGB phase transition’ in Magellanic Cloud clusters is used to calibrate the contribution of the thermally pulsing asymptotic giant branch phase to the synthetic integrated luminosity. As an illustrative example, solar-metallicity (Y = 0.27, Z = 0.02) models, with ages ranging between 30 Myr and 15 Gyr and various choices for the slope of the initial mass function, are presented. Synthetic broad-band colours and the luminosity contributions of the various evolutionary stages are compared with Large Magellanic Cloud and Galactic globular cluster data. In all these cases, a good agreement is found. Finally, the evolution is presented of stellar mass-to-light ratios in the bolometric and UBVRK passbands, in which the contribution of stellar remnants is accounted for.