  The rotation rates in the deep interior and at the surface of 22
main-sequence stars with masses between $1.0$ and $1.6\,{\rm M}_{\odot}$ are
constrained by combining asteroseismological analysis with spectroscopic
measurements. The asteroseismic data of each star are taken by the {\it Kepler}
or CoRoT space mission. It is found that the difference between the surface
rotation rate and the average rotation rate (excluding the convective core) of
most of stars is small enough to suggest that an efficient process of angular
momentum transport operates during and/or before the main-sequence stage of
stars. If each of the surface convective zone and the underlying radiative
zone, for individual stars, is assumed to rotate uniformly, the difference in
the rotation rate between the two zones turns out to be no more than a factor
of two in most of the stars independently of their ages.
