  Rotational shear in Sun-like stars is thought to be an important ingredient
in models of stellar dynamos. Thanks to helioseismology, rotation in the Sun is
characterized well, but the interior rotation profiles of other Sun-like stars
are not so well constrained. Until recently, measurements of rotation in
Sun-like stars have focused on the mean rotation, but little progress has been
made on measuring or even placing limits on differential rotation. Using
asteroseismic measurements of rotation we aim to constrain the radial shear in
five Sun-like stars observed by the NASA Kepler mission: KIC004914923,
KIC005184732, KIC006116048, KIC006933899, and KIC010963065. We used stellar
structure models for these five stars from previous works. These models provide
the mass density, mode eigenfunctions, and the convection zone depth, which we
used to compute the sensitivity kernels for the rotational frequency splitting
of the modes. We used these kernels as weights in a parametric model of the
stellar rotation profile of each star, where we allowed different rotation
rates for the radiative interior and the convective envelope. This parametric
model was incorporated into a fit to the oscillation power spectrum of each of
the five Kepler stars. This fit included a prior on the rotation of the
envelope, estimated from the rotation of surface magnetic activity measured
from the photometric variability. The asteroseismic measurements without the
application of priors are unable to place meaningful limits on the radial
shear. Using a prior on the envelope rotation enables us to constrain the
interior rotation rate and thus the radial shear. In the five cases that we
studied, the interior rotation rate does not differ from the envelope by more
than approximately +/-30%. Uncertainties in the rotational splittings are too
large to unambiguously determine the sign of the radial shear.
