  Recently, by analysing the oscillation frequencies of 90 stars, Yildiz,
\c{C}elik Orhan & Kayhan have shown that the reference frequencies ($\nu_{\rm
min0}$, $\nu_{\rm min1}$ and $\nu_{\rm min2}$) derived from glitches due to He
{\scriptsize II} ionization zone have very strong diagnostic potential for the
determination of their effective temperatures. In this study, we continue to
analyse the same stars and compute their mass, radius and age from different
scaling relations including relations based on $\nu_{\rm min0}$, $\nu_{\rm
min1}$ and $\nu_{\rm min2}$. For most of the stars, the masses computed using
$\nu_{\rm min0}$ and $\nu_{\rm min1}$ are very close to each other. For 38
stars, the difference between these masses is less than 0.024 ${\rm M}_\odot$.
The radii of these stars from $\nu_{\rm min0}$ and $\nu_{\rm min1}$ are even
closer, with differences of less than 0.007 ${\rm R}_\odot$. These stars may be
the most well known solar-like oscillating stars and deserve to be studied in
detail. The asteroseismic expressions we derive for mass and radius show slight
dependence on metallicity. We therefore develop a new method for computing
initial metallicity from this surface metallicity by taking into account the
effect of microscopic diffusion. The time dependence of initial metallicity
shows some very interesting features that may be important for our
understanding of chemical enrichment of Galactic Disc. According to our
findings, every epoch of the disc has its own lowest and highest values for
metallicity. It seems that rotational velocity is inversely proportional to 1/2
power of age as given by the Skumanich relation.
