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

Nearly-uniform internal rotation of solar-like main-sequence stars revealed by space-based asteroseismology and spectroscopic measurements