Visual Orbits of Spectroscopic Binaries with the CHARA Array. I. HD 224355

TL;DR

This paper combines interferometric and spectroscopic data to determine the detailed orbital and physical parameters of the binary star HD 224355, providing insights into stellar evolution at the end of the main sequence.

Contribution

First combined visual and spectroscopic orbit analysis of HD 224355, refining stellar masses, radii, and age estimates with high precision.

Findings

Component masses are approximately 1.63 and 1.61 solar masses.

Estimated stellar radii are about 2.65 and 2.47 solar radii.

Both stars are nearing the end of the main sequence at around 1.9 Gyr.

Abstract

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 M1 = 1.626 +/- 0.005 Msun and M2 = 1.608 +/- 0.005 Msun, and a distance of d = 63.98 +/- 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 R1 = 2.65 +/- 0.21 Rsun and R2 = 2.47 +/- 0.23 Rsun. 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.