  Asteroseismic measurements of the internal rotation rate in evolved stars
pointed out to a lack of angular momentum (AM) transport in stellar evolution
models. Several physical processes in addition to hydrodynamical ones were
proposed as candidates for the missing mechanism. Nonetheless, no current
candidate can satisfy all the constraints provided by asteroseismology. We
revisit the role of a candidate process whose efficiency scales with the
contrast between the rotation rate of the core and the surface which was
proposed to be related to the azimuthal magneto-rotational instability (AMRI)
by Spada et al. We compute stellar evolution models of low- and
intermediate-mass stars with the parametric formulation of AM transport
proposed by Spada et al. until the end of the core-helium burning for low- and
intermediate-mass stars and compare our results to the latest asteroseismic
constraints available in the post main sequence phase. Both hydrogen-shell
burning stars in the red giant branch and core-helium burning stars of low- and
intermediate-mass in the mass range $1 M_{\odot} \lesssim M \lesssim 2.5
M_{\odot}$ can be simultaneously reproduced by this kind of parametrisation.
Given current constraints from asteroseismology, the core rotation rate of
post-main sequence stars seems to be well explained by a process whose
efficiency is regulated by the internal degree of differential rotation in
radiative zones.
