Absolute dimensions of the low-mass eclipsing binary system NSVS 10653195^⋆

¹ Astrophysics Department, Universidad de La Laguna, 38205 La Laguna, Tenerife, Spain
² Centro de Estudios de Física del Cosmos de Aragón, Plaza San Juan 1, 44001 Teruel, Spain
e-mail: riglesias@cefca.es
³ Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain
⁴ Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
⁵ NASA AMES Research Center, Moffet Field, CA, USA

Received: 20 March 2019
Accepted: 5 June 2019

Abstract

Context. Low-mass stars in eclipsing binary systems show radii larger and effective temperatures lower than theoretical stellar models predict for isolated stars with the same masses. Eclipsing binaries with low-mass components are hard to find due to their low luminosity. As a consequence, the analysis of the known low-mass eclipsing systems is key to understand this behavior.

Aims. We aim to investigate the mass–radius relation for low-mass stars and the cause of the deviation of the observed radii in low-mass detached eclipsing binary stars (LMDEB) from theoretical stellar models.

Methods. We developed a physical model of the LMDEB system NSVS 10653195 to accurately measure the masses and radii of the components. We obtained several high-resolution spectra in order to fit a spectroscopic orbit. Standardized absolute photometry was obtained to measure reliable color indices and to measure the mean T_eff of the system in out-of-eclipse phases. We observed and analyzed optical VRI and infrared JK band differential light-curves which were fitted using PHOEBE. A Markov chain Monte-Carlo (MCMC) simulation near the solution found provides robust uncertainties for the fitted parameters.

Results. NSVS 10653195 is a detached eclipsing binary composed of two similar stars with masses of M₁ = 0.6402 ± 0.0052 M_⊙ and M₂ = 0.6511 ± 0.0052 M_⊙ and radii of R₁ = 0.687^+0.017_−0.024 R_⊙ and R₂ = 0.672^+0.018_−0.022 R_⊙. Spectral types were estimated to be K6V and K7V. These stars rotate in a circular orbit with an orbital inclination of i = 86.22 ± 0.61 degrees and a period of P = 0.5607222(2) d. The distance to the system is estimated to be d = 135.2^+7.6_−7.9 pc, in excellent agreement with the value from Gaia. If solar metallicity were assumed, the age of the system would be older than log (age) ∼ 8 based on the M_bol–log T_eff diagram.

Conclusions. NSVS 10653195 is composed of two oversized and active K stars. While their radii is above model predictions their T_eff are in better agreement with models.