Asteroseismic diagnostics of stellar convective cores
Asteroseismic diagnostics of stellar convective cores
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DOI：
10.1111/j.1365-2966.2006.10912.x
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发表时间：
2005-12
影响因子：
4.8
通讯作者：
A. Mazumdar;S. Basu;B. L. Collier;P. Demarque
中科院分区：
文献类型：
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作者：
A. Mazumdar;S. Basu;B. L. Collier;P. Demarque
我们提出了一个详细的研究的小频率分离的对流核心的质量和太阳型恒星的演化阶段的诊断。我们演示了如何将小的分离相结合，以提供敏感的测试对流过冲的核心边缘的存在。这些研究集中在低度振荡模式上，这是预计在遥远恒星中检测到的唯一模式。使用模拟数据与现实的错误，我们发现，对流核心的质量可以估计到5%以内，如果总恒星质量是已知的。由于质量的不确定性而产生的系统误差可能高达20%.The演化阶段的星星，确定的中心氢丰度使用我们提出的技术，但是，是不太敏感的质量估计。
We present a detailed study of the small frequency separations as diagnostics of the mass of the convective core and evolutionary stage of solar-type stars. We demonstrate how the small separations can be combined to provide sensitive tests for the presence of convective overshoot at the edge of the core. These studies are focused on low-degree oscillation modes, the only modes expected to be detected in distant stars. Using simulated data with realistic errors, we find that the mass of the convective core can be estimated to within 5 per cent if the total stellar mass is known. Systematic errors arising due to uncertainty in the mass could be up to 20 per cent. The evolutionary stage of the star, determined in terms of the central hydrogen abundance using our proposed technique, however, is much less sensitive to the mass estimate.