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The internal angular momentum distribution of a star is key to determine itsevolution. Fortunately, the stellar internal rotation can be probed throughstudies of rotationally-split non-radial oscillation modes. In particular,detection of non-radial gravity modes (g modes) in massive young stars hasbecome feasible recently thanks to the Kepler space mission. Our aim is toderive the internal rotation profile of the Kepler B8V star KIC 10526294through asteroseismology. We interpret the observed rotational splittings ofits dipole g modes using four different approaches based on the best seismicmodels of the star and their rotational kernels. We show that these kernels canresolve differential rotation the radiative envelope if a smooth rotationalprofile is assumed and the observational errors are small. Based on Keplerdata, we find that the rotation rate near the core-envelope boundary is wellconstrained to $163\pm89$ nHz. The seismic data are consistent with rigidrotation but a profile with counter-rotation within the envelope has astatistical advantage over constant rotation. Our study should be repeated forother massive stars with a variety of stellar parameters in order to deduce thephysical conditions that determine the internal rotation profile of youngmassive stars, with the aim to improve the input physics of their models.

The internal rotation profile of the B-type star KIC10526294 from frequency inversion of its dipole gravity modes and statistical model comparison