The internal angular momentum distribution of a star is key to determine its evolution . Fortunately , the stellar internal rotation can be probed through studies of rotationally-split nonradial oscillation modes . In particular , detection of nonradial gravity modes ( g modes ) in massive young stars has become feasible recently thanks to the Kepler space mission . Our aim is to derive the internal rotation profile of the Kepler B8V star KIC 10526294 through asteroseismology . We interpret the observed rotational splittings of its dipole g modes using four different approaches based on the best seismic models of the star and their rotational kernels . We show that these kernels can resolve differential rotation within the radiative envelope if a smooth rotational profile is assumed and the observational errors are small . Based on Kepler data , we find that the rotation rate near the core-envelope boundary is well constrained to 163 \pm 89 nHz . The seismic data are consistent with rigid rotation but a profile with counter-rotation within the envelope has a statistical advantage over constant rotation . Our study should be repeated for other massive stars with a variety of stellar parameters in order to deduce the physical conditions that determine the internal rotation profile of young massive stars , with the aim to improve the input physics of their models .