  Understanding differential rotation of Sun-like stars is of great importance
for insight into the angular momentum transport in these stars. One means of
gaining such information is that of asteroseismology. By a forward modeling
approach we analyze in a qualitative manner the impact of different
differential rotation profiles on the splittings of p-mode oscillation
frequencies. The optimum modes for inference on differential rotation are
identified along with the best value of the stellar inclination angle. We find
that in general it is not likely that asteroseismology can be used to make an
unambiguous distinction between a rotation profile such as, e.g., a conical
Sun-like profile and a cylindrical profile. In addition, it seems unlikely that
asteroseismology of Sun-like stars will result in inferences on the radial
profile of the differential rotation, such as can be done for, e.g., red
giants. At best one could possibly obtain the sign of the radial differential
rotation gradient. Measurements of the extent of the latitudinal differential
from frequency splitting are, however, more promising. One very interesting
aspect that could likely be tested from frequency splittings is whether the
differential rotation is solar-like or anti-solar-like in nature, in the sense
that a solar-like profile has an equator rotating faster than the poles.
