  The radial gradient of the rotation rate in the near-surface shear layer
(NSSL) of the Sun is independent of latitude and radius. Theoretical mean-field
models have been successful in explaining this property of the solar NSSL,
while global direct convection models have been unsuccessful. We investigate
reason for this discrepancy by measuring the mean flows, Reynolds stress, and
turbulent transport coefficients under NSSL conditions. Simulations have
minimal ingredients. These ingredients are inhomogeneity due to boundaries,
anisotropic turbulence, and rotation. Parameters of the simulations are chosen
such they match the weakly rotationally constrained NSSL. The simulations probe
locally Cartesian patches of the star at a given depth and latitude. The depth
of the patch is varied by changing the rotation rate such that the resulting
Coriolis numbers<1. We measure the turbulent transport coefficient relevant for
the non-diffusive and diffusive parts of the Reynolds stress and compare them
with predictions of current mean-field theories. A negative radial gradient of
mean flow similar to the solar NSSL is generated only at the equator where
meridional flows are absent. At other latitudes the meridional flow is
comparable to the mean flow corresponding to differential rotation. We also
find that meridional components of the Reynolds stress cannot be ignored.
Additionally, we find that the turbulent viscosity is quenched by rotation by
about 50\% from the surface to the bottom of the NSSL. Our local simulations do
not validate the explanation for the generation of the NSSL from mean-field
theory where meridional stresses are neglected. However, the rotational
dependence of turbulent viscosity in our simulations is in good agreement with
theoretical prediction. Our results are in qualitative agreement with global
convection simulations in that a NSSL obtained near the equator.
