  Standard solar models (SSMs) constructed in accordance with old solar
abundances are in reasonable agreement with seismically inferred results, but
SSMs with new low-metal abundances disagree with the seismically inferred
results. The constraints of neutrino fluxes on solar models exist in parallel
with those of helioseismic results. The solar neutrino fluxes were updated by
Borexino Collaboration. We constructed rotating solar models with new low-metal
abundances where the effects of enhanced diffusion and convection overshoot
were included. A rotating model using OPAL opacities and the Caffau abundance
scale has better sound-speed and density profiles than the SSM with the old
solar abundances and reproduces the observed $p$-mode frequency ratios $r_{02}$
and $r_{13}$. The depth and helium abundance of the convection zone of the
model agree with the seismically inferred ones at the level of $1\sigma$. The
updated neutrino fluxes are also reproduced by the model at the level of
$1\sigma$. The effects of rotation and enhanced diffusion not only improve the
model's sound-speed and density profiles but bring the neutrino fluxes
predicted by the model into agreement with the detected ones. Moreover, the
calculations show that OP may underestimate opacities for the regions of the
Sun with $T\gtrsim5\times10^{6}$ K by around $1.5\%$, while OPAL may
underestimate opacities for the regions of the Sun with $2\times10^{6}$ K
$\lesssim T \lesssim 5\times10^{6}$ K by about $1-2\%$.

Solar and Stellar Astrophysics;Nuclear Theory