Rediscussion of eclipsing binaries. Paper XXII. The B-type system MU Cassiopeiae

TL;DR

This study analyzes the physical properties of the B-type eclipsing binary MU Cas using TESS light curves and spectroscopic data, confirming stellar parameters and evolutionary status, with some discrepancies in distance measurements.

Contribution

It provides updated measurements of stellar masses, radii, and distance for MU Cas, and compares these with theoretical models, highlighting the need for further spectroscopic analysis.

Findings

Stellar masses: ~4.6 Msun for both stars

Radii: ~4.1 and 3.65 Rsun for primary and secondary

Distance: 1814 +/- 37 pc, slightly shorter than Gaia DR3 estimate

Abstract

MU Cas is a detached eclipsing binary containing two B5 V stars in an orbit of period 9.653 d and eccentricity 0.192, which has been observed in seven sectors using the Transiting Exoplanet Survey Satellite (TESS). We use these new light curves together with published spectroscopic results to measure the physical properties of the component stars, finding masses of 4.67 +/- 0.09 Msun and 4.59 +/- 0.08 Msun, and radii of 4.12 +/- 0.04 Rsun and 3.65 +/- 0.05 Rsun. These values agree with previous results save for a change in which of the two stars is designated the primary component. The measured distance to the system, 1814 +/- 37 pc, is 1.8$\sigma$ shorter than the distance from the Gaia DR3 parallax. A detailed spectroscopic analysis of the system is needed to obtain improved temperature and radial velocity measurements for the component stars; a precise spectroscopic light ratio is also required for better measurement of the stellar radii. MU Cas matches the predictions of theoretical stellar evolutionary models for a solar chemical composition and an age of 87 +/- 5 Myr. No evidence for pulsations was found in the light curves.