We present the visual orbit of the double-lined spectroscopic binary HD 224355 from interferometric observations with the CHARA Array , as well as an updated spectroscopic analysis using echelle spectra from the Apache Point Observatory 3.5m telescope .
By combining the visual and spectroscopic orbital solutions , we find the binary components to have masses of M _ { 1 } = 1.626 \pm 0.005 M _ { \odot } and M _ { 2 } = 1.608 \pm 0.005 M _ { \odot } , and a distance of d = 63.98 \pm 0.26 pc .
Using the distance and the component angular diameters found by fitting spectrophotometry from the literature to spectral energy distribution models , we estimate the stellar radii to be R _ { 1 } = 2.65 \pm 0.21 R _ { \odot } and R _ { 2 } = 2.47 \pm 0.23 R _ { \odot } .
We then compare these observed fundamental parameters to the predictions of stellar evolution models , finding that both components are evolved towards the end of the main sequence with an estimated age of 1.9 Gyr .