恒星参数的干涉测量研究：金属丰度A型双星β Aur的质量
Interferometric Survey of Stellar Parameters: Mass of the metallic A-type binary $β$ Aur
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中文总结 AI 辅助
本研究利用CHARA/SPICA等多源观测数据，通过联合建模推导了A型食双星β Aur的轨道、质量、半径及距离等恒星参数，验证了多观测融合方法的可靠性。
中文摘要 AI 辅助
凭借新型可见光CHARA/SPICA仪器的能力以及CHARA的多光谱波段操作，我们的目标是解析短周期双星的轨道，并开发一套将干涉测量、光谱学和测光观测结合为单一一致模型的可靠框架。基于CHARA/SPICA仪器的预期性能，我们根据亮度、角距离和轨道特性选择了合适的双星作为目标样本。作为案例研究，我们分析了明亮的食双星御夫座β（β Aurigae），它由两颗略微演化的A1型恒星组成。我们将用CHARA/SPICA、MIRC-X和MYSTIC获得的β Aur的新干涉测量观测数据，与存档的MIRC数据、视向速度和光曲线相结合。我们首先从干涉测量观测量中推导天体测量位置并计算轨道解，之后实现了一个统一模型，该模型能够将干涉测量建模与ellc代码关联，以使用MCMC采样同时拟合所有观测量。我们对每个数据集的噪声统计进行了详细分析，最终采用轮廓似然方法来解决低估噪声和系统误差的问题。我们通过联合建模推导了β Aur的一致轨道和物理解。干涉测量数据的加入严格约束了角半长轴和倾角。通过使用轮廓似然处理本质不同的观测量的固有不确定性水平差异，我们得出了两颗恒星的质量：M₁ = 2.359 ± 0.005 M_S，M₂ = 2.293 ± 0.004 M_S；它们的半径：R₁ = 2.752 ± 0.002 R_S，R₂ = 2.622 ± 0.002 R_S；以及该双星的距离：d = 24.30 ± 0.05 pc。
英文摘要
With the capabilities of the new visible CHARA/SPICA instrument and the multiple spectral band operation of CHARA, our goal is to resolve orbits of short-period binaries and develop a robust framework for combining interferometric, spectroscopic, and photometric observations into a single consistent model. For our target sample, we selected suitable binaries based on brightness, angular separation, and orbital properties based on the expected performance of the CHARA/SPICA instrument. As a case study, we analysed the bright eclipsing binary $β$ Aurigae, composed of two slightly evolved A1 stars. We combined new interferometric observations of $β$ Aur obtained with CHARA/SPICA, MIRC-X, and MYSTIC with archival MIRC data, radial velocities, and light curves. We first derived astrometric positions from interferometric observables and computed an orbital solution. Afterwards, we implemented a unified model, capable of tying interferometric modelling with the ellc code to simultaneously fit all observables using MCMC sampling. We performed a detailed analysis of the noise statistics of each data set and in the end we adopted a profile likelihood approach to account for underestimated noise and systematics. We derived a consistent orbital and physical solution for $β$ Aur through joint modelling. The inclusion of interferometric data tightly constrains the angular semi-major axis and inclination. Using profile likelihood to account for the different intrinsic levels of uncertainty of the fundamentally different observables, we derived the masses of the two stars, $M_1 = 2.359 \pm 0.005$ M$_S$ and $M_2 = 2.293 \pm 0.004$ M$_S$, their radii $R_1 = 2.752 \pm 0.002$ R$_S$ and $R_2 = 2.622 \pm 0.002$ R$_S$, and the distance to the binary, $d = 24.30\pm0.05$ pc.
发表机构
- Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Laboratoire Lagrange（蔚蓝海岸大学，蔚蓝海岸天文台）
- Astronomy Department, University of Michigan（密歇根大学天文学系）
- Charles University, Faculty of Mathematics and Physics, Astronomical Institute（查理大学数学物理学院天文研究所）
- GAPHE, STAR, Université de Liège（列日大学 GAPHE、STAR 研究组）
- The CHARA Array of Georgia State University, Mount Wilson Observatory（佐治亚州立大学 CHARA 阵列，威尔逊山天文台）
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