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.

中文翻译：

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使用 CHARA 阵列的光谱双星的视觉轨道。三、高清 8374 和高清 24546

我们使用 CHARA 阵列和 Palomar 试验台干涉仪获得的干涉观测，展示了两颗长周期分光双星 HD 8374 和 HD 24546 的视觉轨道。我们还使用 APO 3.5 m 和 Fairborn 2.0 m 望远镜从阶梯光谱中获得了新的径向速度。通过结合视觉和光谱观测，我们求解了完整的三维轨道，并将恒星质量和距离确定在 3% 的不确定性内。然后我们通过多普勒断层扫描和光谱能量分布分析估计每个组成恒星的有效温度和半径，以便将观测到的恒星参数与恒星演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 的质量，R1 的半径 = 1.84 +/- 0。05 Rsun 和 R2 = 1.66 +/- 0.12 Rsun，Teff1 = 7280 +/- 110 K 和 Teff2 = 7280 +/- 120 K，估计年龄为 1.0 Gyr。对于 HD 24546，我们发现质量 M1 = 1.434 +/- 0.014 Msun 和 M2 = 1.409 +/- 0.014 Msun，R1 的半径 = 1.67 +/- 0.06 Rsun 和 R2 = 1.60 +/- 0.10 Rsun，温度 Teff1 = 6790 +/- 120 K 和 Teff2 = 6770 +/- 90 K，估计年龄为 1.4 Gyr。因此，HD 24546 太老了，不能成为 Hyades 星团的成员，尽管它在物理上很接近这个群体。估计年龄为 1.4 Gyr。因此，HD 24546 太老了，不能成为 Hyades 星团的成员，尽管它在物理上很接近这个群体。估计年龄为 1.4 Gyr。因此，HD 24546 太老了，不能成为 Hyades 星团的成员，尽管它在物理上靠近该组。