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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 ± 0.050M⊙ and M2 = 1.587 ± 0.049M⊙, radii of R1 = 1.84 ± 0.05R⊙ and R2 = 1.66 ± 0.12R⊙, temperatures of ${T}_{\mathrm{eff}1}=7280\pm 110$ K and ${T}_{\mathrm{eff}2}=7280\pm 120$ K, and an estimated age of 1.0 Gyr. For HD 24546, we find masses of M1 = 1.434 ± 0.014M⊙ and M2 = 1.409 ± 0.014M⊙, radii of R1 = 1.67 ± 0.06R⊙ and R2 = 1.60 ± 0.10R⊙, temperatures of ${T}_{\mathrm{eff}1}=6790\pm 120$ K and ${T}_{\mathrm{eff}2}=6770\pm 90$ 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.

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