The orbit and fundamental physical parameters of the double-lined eclipsing binary V505 Per are derived by means of Echelle high resolution , high S/N spectroscopy and B , V photometry .
In addition , effective temperatures , gravities , rotational velocities and metallicities of both components are obtained also from atmospheric \chi ^ { 2 } analysis , showing excellent match with the results of orbital solution .
An E _ { B - V } \leq 0.01 mag upper limit to the reddening is derived from intensity analysis of interstellar NaI ( 5890.0 & 5895.9 Å ) and KI ( 7699.0 Å ) lines .
The distance to the system computed from orbital parameters ( 60.6 \pm 1 pc ) is identical to the newly re-reduced Hipparcos parallax ( 61.5 \pm 1.9 pc . ) .
The masses of the two components ( M _ { 1 } =1.2693 \pm 0.0011 and M _ { 2 } =1.2514 \pm 0.0012 M _ { \odot } ) place them in the transition region between convective and radiative stellar cores of the HR diagram , with the more massive of the two showing already the effect of evolution within the Main Sequence band ( T _ { 1 } =6512 \pm 21 K , T _ { 2 } =6462 \pm 12 K , R _ { 1 } =1.287 \pm 0.014 , R _ { 2 } =1.266 \pm 0.013 R _ { \odot } ) .
This makes this system of particular relevance to theoretical stellar models , as a test on the overshooting .
We compare the firm observational results for V505 Per component stars with the predictions of various libraries of theoretical stellar models ( BaSTI , Padova , Granada , Yonsei-Yale , Victoria-Regina ) as well as BaSTI models computed specifically for the masses and chemical abundances of V505 Per .
We found that the overshooting at 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 1.25 M _ { \odot } components , respectively .
According to the computed BaSTI models , the age of the system is \sim 0.9 Gyr and the element diffusion during this time has reduced 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 \pm 0.03 .