  Helioseismic observations have revealed many properties of the Sun: the depth
and the helium abundance of the convection zone, the sound-speed and the
density profiles in the solar interior. Those constraints have been used to
judge the stellar evolution theory. With the old solar composition (e.g.,
GS98), the solar standard model is in reasonable agreement with the
helioseismic constraints. However, a solar model with revised composition
(e.g., AGSS09) with low abundance $Z$ of heavy elements cannot be consistent
with those constraints. This is the so-called "solar abundance problem",
standing for more than ten years even with the recent upward revised Ne
abundance. Many mechanisms have been proposed to mitigate the problem. However,
there is still not a low-$Z$ solar model satisfying all helioseismic
constraints. In this paper, we report a possible solution to the solar
abundance problem. With some extra physical processes that are not included in
the standard model, solar models can be significantly improved. Our new solar
models with convective overshoot, the solar wind, and an early mass accretion
show consistency with helioseismic constraints, the solar Li abundance, and
observations of solar neutrino fluxes.
