The orbital elements and physical properties of the eclipsing binary BD+36°3317, a probable member of δ Lyrae cluster

Context. The fact that eclipsing binaries belong to a stellar group is useful, because the former can be used to estimate distance and additional properties of the latter, and vice versa. Aims. Our goal is to analyse new spectroscopic observations of BL+36 degrees 3317 along with the photometric observations from the literature and, for the first time, to derive all basic physical properties of this binary. We aim to find out whether the binary is indeed a member of the delta Lyr open cluster. Methods. The spectra were reduced using the IRAF program and the radial velocities were measured with the program SPEFO. The line spectra of both components were disentangled with the program KOREL and compared to a grid of synthetic spectra. The final combined radial-velocity and photometric solution was obtained with the program PHOEBE. Results. We obtained the following physical elements of BD+36 degrees 3317: M-1 = 2.24 +/- 0.07 M-circle dot, M-2 = 1.52 +/- 0.03 M-circle dot, R-1= 1.76 +/- 0.01 R-circle dot, R-2 = 1.46 +/- 0.01 R-circle dot, log L-1 = 1.52 +/- 0.08 L-circle dot log L-2 = 0.81 +/- 0.07 L-circle dot. We derived the effective temperatures T-eff,T-1 = 10 450 +/- 420 K, T-eff,T-2 = 7623 +/- 328 K. Both components are located close to zero age main sequence in the Hertzsprung-Russell (HR) diagram and their masses and radii are consistent with the predictions of stellar evolutionary models. Our results imply the average distance to the system (d) over bar = 330 +/- 29 pc. We re-investigated the membership of BD+36 degrees 3317 in the delta Lyr cluster and confirmed it. The distance to BD+36 degrees 3317, given above, therefore represents an accurate estimate of the true distance for delta Lyr cluster. Conclusions. The reality of the delta Lyr cluster and the cluster membership of BD+36 degrees 3317 have been reinforced.