  The ratio of metal abundance to hydrogen abundance of the solar photosphere,
$(Z/X)_{s}$, has been revised several times. Standard solar models, based on
these revised solar abundances, are in disagreement with seismically inferred
results. Recently, Magg et al. introduced a new value for $(Z/X)_{s}$, which is
still in debate in the community. The solar abundance problem or solar modeling
problem remains a topic of ongoing debate. We constructed rotating solar models
in accordance with various abundance scales where the effects of convection
overshoot and enhanced diffusion were included. Among these models, those
utilizing Magg's abundance scale exhibit superior sound-speed and density
profiles compared to models using other abundance scales. Additionally, they
reproduce the observed frequency separation ratios $r_{02}$ and $r_{13}$. These
models also match the seismically inferred surface helium abundance and
convection zone depth within $1\sigma$ level. Furthermore, the calculated
neutrino fluxes from these models agree with detected ones at the level of
$1\sigma$. We found that neutrino fluxes and density profile are influenced by
nuclear reactions, allowing us to use the combination of detected neutrino
fluxes and seismically inferred density for diagnosing astrophysical
$S$-factors. This diagnostic approach shows that $S_{11}$ may be underestimated
by $2\%$, while $S_{33}$ may be overestimated by about $3\%$ in previous
determinations. The $S$-factors favored by updated neutrino fluxes and
helioseismic results can lead to significant improvements in solar models.
