  The details of the dynamo process in the Sun are an important aspect of
research in solar-terrestrial physics and astrophysics. The surface part of the
dynamo can be constrained by direct observations, but the subsurface part lacks
direct observational constraints. The torsional oscillations, a small periodic
variation of the Sun's rotation with the solar cycle, are thought to result
from the Lorentz force of the cyclic magnetic field generated by the dynamo. In
this study, we aim to discriminate between three Babcock-Leighton (BL) dynamo
models by comparing the zonal acceleration of the three models with the
observed one. The property that the poleward and equatorward branches of the
torsional oscillations originate from about $\pm 55^\circ$ latitudes with their
own migration time periods serves as an effective discriminator that could
constrain the configuration of the magnetic field in the convection zone. The
toroidal field, comprising poleward and equatorward branches separated at about
$\pm 55^\circ$ latitudes can generate the two branches of the torsional
oscillations. The alternating acceleration and deceleration bands in time is
the other property of the torsional oscillations that discriminate between the
dynamo models. To reproduce this property, the phase difference between the
radial ($B_{r}$) and toroidal ($B_{\phi}$) components of the magnetic field
near the surface should be about $\pi/2$.
