The mass and radius of the M-dwarf companion in the double-lined eclipsing binary T-Cyg1-01385

TL;DR

This study spectroscopically characterizes the eclipsing binary T-Cyg1-01385, revealing the masses and radii of both stars, including a low-mass M-dwarf companion near the transition to full convection, and compares findings with stellar models.

Contribution

First spectroscopic detection of both components in T-Cyg1-01385, providing precise physical parameters and insights into the low-mass star transition region.

Findings

Masses: M1=1.059±0.032 M☉, M2=0.342±0.017 M☉

Radii: R1=1.989±0.022 R☉, R2=0.457±0.013 R☉

Secondary near transition from partial to full convection

Abstract

We observed spectroscopically the eclipsing binary system T-Cyg1-01385 in order to determine physical properties of the components. The double-lined nature of the system is revealed for the first time and the radial velocities are obtained for both stars. We have derived masses, radii and luminosities for both components. Analyses of the radial velocities and the KeplerCam and the T$r$ES light curves yielded masses of M$_1$=1.059$\pm$0.032 \Msun ~and M$_2$=0.342$\pm$0.017 {\Msun} and radii of R$_1$=1.989$\pm$0.022 {\Rsun} and R$_2$=0.457$\pm$0.013 {\Rsun}. Locations of the low-mass companion in the mass-radius and mass-effective temperature planes and comparison with the other low-mass stars show that the secondary star appears just at the transition from partially to fully convective interiors for the M dwarfs. When compared to stellar evolution models, the luminosities and effective temperatures of the components are consistent with Z=0.004 and an age of about 6 Gyr. A distance to the system was calculated as d=355$\pm$7 pc using the BV and JHK magnitudes.