  HD 129929 is a slowly-rotating $\beta$ Cephei pulsator with a rich spectrum
of detected oscillations, including two rotational multiplets. The
asteroseismic interpretation revealed the presence of radial differential
rotation in this massive star of $\sim$9.35 M . The stellar core is indeed
estimated to spin $\sim$3.6 times faster than the surface. The surface rotation
was consequently derived as $\sim$2 km/s. This massive star represents an ideal
counter-part to the wealth of space-based photometry results for main-sequence
and evolved low-mass stars. Those latter have revealed a new, and often
unexpected, picture of the angular momentum transport processes acting in
stellar interiors. We investigate in a new way the constraints on the internal
rotation of HD 129929, focusing on their interpretation for the evolution of
the internal rotation during the main sequence of a massive star. We test
separately hydrodynamic and magnetic instability transport processes of angular
momentum. We used the best asteroseismic model obtained in an earlier work. We
calibrated stellar models including rotation, with different transport
processes, to reproduce that reference model. We then looked whether one
process is favoured to reproduce the rotation profile of HD 129929, based on
the fit of the asteroseismic multiplets. The impact of the Tayler magnetic
instability on the angular momentum transport predicts a ratio of the
core-to-surface rotation rate of only 1.6, while the recently revised
prescription of this mechanism predicts solid-body rotation. Both are too low
in comparison with the asteroseismic inference. The models with only
hydrodynamic processes are in good agreement with the asteroseismic
measurements. Strikingly, we can also get a constraint on the profile of
rotation on the zero age main sequence: likely, the ratio between the core and
surface rotation was at least $\sim$1.7.
