Rediscussion of eclipsing binaries. Paper XXVIII. The metallic-lined system DV Bootes

TL;DR

This study precisely characterizes the physical properties of the eclipsing binary DV Bootes, combining TESS photometry and spectroscopy, revealing insights into its stellar parameters, distance, age, and metallicity, with some discrepancies noted.

Contribution

First detailed analysis of the metallic-lined binary DV Bootes using TESS and spectroscopic data, providing high-precision stellar parameters and metallicity insights.

Findings

Masses of 1.617 and 1.207 solar masses for primary and secondary.

Radii of 1.948 and 1.195 solar radii, with measurement limitations.

Distance of 125.0 parsecs, consistent with Gaia data.

Abstract

DV Boo is a detached eclipsing binary containing a metallic-lined A-star and a chemically normal late-F star, in an orbit with a period of 3.783 d and a possible slight eccentricity. We use a light curve from the Transiting Exoplanet Survey Satellite (TESS) and published spectroscopic results to determine the physical properties of the system to high precision. We find masses of 1.617 +/- 0.003 Msun and 1.207 +/- 0.004 Msun, and radii of 1.948 +/- 0.008 Rsun and 1.195 +/- 0.022 Rsun. The precision of the radius measurements is limited by the shallow partial eclipses and the unavailability of a spectroscopic light ratio due to the chemical peculiarity of the primary star. We measure a distance to the system of 125.0 +/- 1.5 pc, in good agreement with the Gaia DR3 parallax, and an age of 1.3 Gyr. A comparison with theoretical models suggests the system has a modestly sub-solar metallicity, in conflict with the slightly super-solar photospheric abundances of the secondary star.