  Asteroseismology has become a powerful tool to study the internal rotation of
stars, and its study allows to constrain the internal AM transport processes
and better understand their physical nature. In this context, we compared the
rotation rates predicted by asteroseismology and by starspots measurements for
four main-sequence stars from the Kepler LEGACY sample, considering different
AM transport prescriptions, and investigated if some of these prescriptions
could be ruled out.
  We decoupled the modelling of the structure and of the rotational profile,
respectively obtained by an asteroseismic characterization and by using
rotating models including a detailed treatment of the AM transport. We then
compared the mean asteroseismic rotation rate with the surface rotation rate
from starspots measurements for each of the AM transport prescriptions. In the
hotter part of the HRD (M > ~ 1.2Msun), combining asteroseismic constraints
from splittings of pressure modes and surface rotation rates does not allow to
conclude on the need for an efficient AM transport in addition to the sole
transport by meridional circulation and shear instability. Both prescriptions
are indeed consistent with the quasi-solid rotation measured by Benomar et al.
(2015) and Nielsen et al. (2017). In the colder part of the HRD, the situation
is different due to the efficient braking of the stellar surface by magnetised
winds. We find a clear disagreement between the rotational properties of models
including only hydrodynamic processes and asteroseismic constraints, while
models with magnetic fields correctly reproduce the observations, similarly to
the solar case.
  This shows the existence of a mass regime corresponding to main-sequence
stars around ~ 6000 - 6200 K for which it is difficult to constrain the AM
transport processes, unlike for hotter, Gamma Dor stars or colder, less massive
solar analogs.
