2018AcA....68..269D

We present the first spectroscopic analysis of the eclipsing binary BD-00°2862. The All Sky Automated Survey light curves yield orbital period of the system of 2.15 d. The shape of the light curve reveals that the components are almost spherical and the binary is detached. The eclipses depths show significant difference of the components' temperature. We acquired spectra with 0.5-m telescope equipped with an echelle spectrograph. The spectra are dominated by the lines of the more luminous component, which is about five times more luminous than its close companion. Obtained radial velocities together with the light curves enabled us to obtain a model of the system using the Wilson-Devinney method. The mass ratio of the stars is 0.67 and the size of the semi-major axis is 8.6 R_☉. The masses of the eclipsing components are M₁=1.08±0.03 M_☉ and M₂=0.72±0.02 M_☉. The stars are not evolved and the radii are close to the main sequence values: R₁=1.21±0.01 R_☉ and R₂=0.71±0.01 R_☉. The evolutionary tracks show that the system is probably on the pre main sequence stage. The photometric parallax yields distance of 131 pc, which is comparable with the one obtained by Gaia mission-130 pc. We carried out a spectrum analysis for the main component obtaining its temperature of 5600±400 K and the metallicity-[M/H]=-0.30±0.20. The star has a visual companion separated by about 12". The companion has proper motion comparable to the one of the main star. Additionally, its distance based on the trigonometric parallax is equal within errors with the distance of component A. Therefore, the companion is probably a part of the system. Its spectral type is M3 and the estimated mass-about 0.3M_☉.