We present the visual orbits of two long period spectroscopic binary stars , HDÂ 8374 and HDÂ 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 3.5Â m and Fairborn 2.0Â 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 HDÂ 8374 , we find masses of M _ { 1 } = 1.636 \pm 0.050 M _ { \odot } and M _ { 2 } = 1.587 \pm 0.049 M _ { \odot } , radii of R _ { 1 } = 1.84 \pm 0.05 R _ { \odot } and R _ { 2 } = 1.66 \pm 0.12 R _ { \odot } , temperatures of T _ { eff 1 } = 7280 \pm 110 K and T _ { eff 2 } = 7280 \pm 120 K , and an estimated age of 1.0 Gyr .
For HDÂ 24546 , we find masses of M _ { 1 } = 1.434 \pm 0.014 M _ { \odot } and M _ { 2 } = 1.409 \pm 0.014 M _ { \odot } , radii of R _ { 1 } = 1.67 \pm 0.06 R _ { \odot } and R _ { 2 } = 1.60 \pm 0.10 R _ { \odot } , temperatures of T _ { eff 1 } = 6790 \pm 120 K and T _ { eff 2 } = 6770 \pm 90 K , and an estimated age of 1.4 Gyr .
HDÂ 24546 is therefore too old to be a member of the Hyades cluster , despite its physical proximity to the group .