Bright Spectroscopic Binaries: II. A study of five systems with orbital periods of P < 500 days

TL;DR

This study analyzes five bright spectroscopic binary systems with orbital periods under 500 days, determining their orbital parameters, stellar properties, and component masses using radial velocities, spectra, Gaia data, and stellar evolution models.

Contribution

It provides detailed orbital and stellar parameters for five binary systems, including secondary masses and orbital inclinations, using a comprehensive multi-method approach.

Findings

All primary stars are evolved giants.

Secondary star masses and orbital inclinations were successfully estimated.

The systems' properties align with stellar evolution models.

Abstract

We present a detailed analysis of five bright spectroscopic binary systems (HD 18665, HD 27131, HD 171852, HD 215550, HD 217427) that have orbital periods of P < 500 days. We determined the complete set of orbital parameters using the toolkit RadVel by analyzing the observed radial velocity curves. To study the properties of the five systems, we also analyzed the intermediate resolution spectra (R = 20,000) observed with the TIGRE telescope and determined the stellar parameters of the primary stars using the toolkit iSpec. With Gaia Early Data Release 3 parallaxes, a correction for interstellar extinction using the 3D dust map, and bolometric corrections, we placed the stars in the Hertzsprung-Russell diagram and compared the positions with stellar evolution tracks calculated with the Eggleton code to determine the masses and ages of the primary stars. They have all evolved to the giant phase. Finally, we were able to determine the masses of the secondary stars and to estimate the orbital inclinations i of the binary systems.