The orbit and physical parameters of the double-lined eclipsing binary V570 Per , discovered by the Hipparcos satellite , are derived with formal errors better than 1 % using high resolution Echelle spectroscopy and B , V photometry .
Atmospheric analysis is performed on spectra at quadrature using synthetic spectroscopy that indicates a [ Fe/H ] =+0.02 \pm 0.05 metallicity .
V570 Per turns out to be a detached system , with shallow eclipses of \Delta B = \Delta V =0.13 mag and a distance of 123 \pm 3 pc , in fine agreement with Hipparcos 117 ^ { 104 } _ { 132 } pc distance .
V570 Per is composed by unperturbed components of F2 and F5 spectral types and masses of 1.457 \pm 0.004 and 1.351 \pm 0.004 M _ { \odot } respectively , which do not show surface activity .
Both components are still within the Main Sequence band and are dynamically relaxed to co-rotation with the orbital motion .
The system is particularly interesting because both components have their masses in the range where transition occurs between convective and radiative cores , and where differences between families of stellar evolutionary tracks show appreciable differences .
The position of the components of V570 Per on the temperature-luminosity plane is compared with Padova , Geneva , Granada and Teramo-04 theoretical stellar models .
The comparison provides different best fit metallicities and ages , with [ Fe/H ] values ranging from +0.07 to +0.18 , and ages from 0.6 to 1.0 Gyr .