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The orbit and fundamental physical parameters of the double-lined eclipsingbinary V505 Per are derived by means of Echelle high resolution, high S/Nspectroscopy and B, V photometry. Effective temperatures, gravities, rotationalvelocities and metallicities are obtained from atmospheric chi^2 analysis. AnE(B-V)<=0.01 mag reddening is derived from interstellar NaI and KI lines. Thedistance to the system computed from orbital parameters (60.6 +/- 1 pc) isidentical to the newly re-reduced Hipparcos parallax (61.5 +/- 1.9 pc). Themasses of the two components (M(1) = 1.2693 +/- 0.0011 and M(2) = 1.2514 +/-0.0012 Msun) place them in the transition region between convective andradiative stellar cores of the HR diagram, with the more massive of the twoshowing already the effect of evolution within the Main Sequence band (T(1) =6512 +/- 21 K, T(2) = 6462 +/- 12 K, R(1) = 1.287 +/- 0.014, R(2) = 1.266 +/-0.013 Rsun). This makes this system of particular relevance to theoreticalstellar models, as a test on the overshooting. We compare the firmobservational results for V505 Per component stars with the predictions ofvarious libraries of theoretical stellar models (BaSTI, Padova, Granada,Yonsei-Yale, Victoria-Regina) as well as BaSTI models computed specifically forthe masses and chemical abundances of V505 Per. We found that the overshootingat the masses of V505 Per component stars is already pretty low, but not null,and described by efficiencies lambda(OV)=0.093 and 0.087 for the 1.27 and 1.25Msun components, respectively. According to the computed BaSTI models, the ageof the system is about 0.9 Gyr and the element diffusion during this time hasreduced the surface metallicity from the initial [M/H]=-0.03 to the current[M/H]=-0.13, in excellent agreement with observed [M/H]=-0.12 +/- 0.03.

Asiago eclipsing binaries program. II. V505 Per