We show that the inclusion of special relativistic corrections in the revised OPAL and MHD equations of state has a significant impact on the helioseismic determination of the solar age .
Models with relativistic corrections included lead to a reduction of about 0.05 - 0.08 \mathrm { Gyr } with respect to those obtained with the old OPAL or MHD EOS .
Our best-fit value is t _ { \mathrm { seis } } = ( 4.57 \pm 0.11 ) \mathrm { Gyr } which is in remarkably good agreement with the meteoritic value for the solar age .
We argue that the inclusion of relativistic corrections is important for probing the evolutionary state of a star by means of the small frequency separations \delta \nu _ { { \ell,n } } = \nu _ { { \ell,n } } - \nu _ { { \ell + 2 ,n - 1 } } , for spherical harmonic degrees \ell = 0 , 1 and radial order n \gg \ell .