论文标题
带有Chara阵列的光谱二进制的视觉轨道。 iii。 HD 8374和HD 24546
Visual Orbits of Spectroscopic Binaries with the CHARA Array. III. HD 8374 and HD 24546
论文作者
论文摘要
我们使用用Chara阵列和Palomar Test台式干涉仪获得的干涉测量值介绍了两个长期光谱二进制恒星HD 8374和HD 24546的视觉轨道。我们还使用APO 3.5 m和Fairborn 2.0 M望远镜从梯形光谱中获得了新的径向速度。通过将视觉和光谱观测结合在一起，我们求解了完整的三维轨道，并确定恒星质量和距离为3％的不确定性。然后，我们通过多普勒断层扫描和光谱能量分布分析来估计每个组件星的有效温度和半径，以将观察到的恒星参数与恒星进化模型的预测进行比较。对于HD 8374，我们发现M1 = 1.636 +/- 0.050 msun和m2 = 1.587 +/- 0.049 msun，R1 = 1.84 +/- 0.05 +/- 0.05 rsun和r2 = 1.66 +/- 0.12 rsun，温度，TEFF1 = 7280 +/110 +/110 +/110 k和tefffffffff1估计年龄为1.0 GYR。对于HD 24546，我们发现M1 = 1.434 +/- 0.014 MSUN和M2 = 1.409 +/- 0.014 MSUN，RADII，R1 = 1.67 +/- 0.06 +/- 0.06 RSUN和R2 = 1.60 +/- 0.10 +/- 0.10 RSUN，温度，TEFF1 = 6790 +/120 +/-- 120-K和TEFFFffffff1估计年龄为1.4 GYR。因此，HD 24546太老了，尽管与该小组的物理相近，但仍无法成为Hyades群集的成员。
We present the visual orbits of two long period spectroscopic binary stars, HD 8374 and HD 24546, using interferometric observations acquired with the CHARA Array and the Palomar Testbed Interferometer. We also obtained new radial velocities from echelle spectra using the APO 3.5 m and Fairborn 2.0 m telescopes. By combining the visual and spectroscopic observations, we solve for the full, three-dimensional orbits and determine the stellar masses and distances to within 3% uncertainty. We then estimate the effective temperature and radius of each component star through Doppler tomography and spectral energy distribution analyses, in order to compare the observed stellar parameters to the predictions of stellar evolution models. For HD 8374, we find masses of M1 = 1.636 +/- 0.050 Msun and M2 = 1.587 +/- 0.049 Msun, radii of R1 = 1.84 +/- 0.05 Rsun and R2 = 1.66 +/- 0.12 Rsun, temperatures of Teff1 = 7280 +/- 110 K and Teff2 = 7280 +/- 120 K, and an estimated age of 1.0 Gyr. For HD 24546, we find masses of M1 = 1.434 +/- 0.014 Msun and M2 = 1.409 +/- 0.014 Msun, radii of R1 = 1.67 +/- 0.06 Rsun and R2 = 1.60 +/- 0.10 Rsun, temperatures of Teff1 = 6790 +/- 120 K and Teff2 = 6770 +/- 90 K, and an estimated age of 1.4 Gyr. HD 24546 is therefore too old to be a member of the Hyades cluster, despite its physical proximity to the group.
