  Context: The internal characteristics of stars, such as their core rotation
rates, are obtained via asteroseismic observations. A comparison of core
rotation rates found in this way with core rotation rates as predicted by
stellar evolution models demonstrate a large discrepancy. This means that there
must be a process of angular momentum transport missing in the current theory
of stellar evolution. A new formalism was recently proposed to fill in for this
missing process, which has the Tayler instability as its starting point
(hereafter referred to as `Fuller-formalism'). Aims: We investigate the effect
of the Fuller-formalism on the internal rotation of stellar models with an
initial mass of 2.5 Mo. Methods: Stellar evolution models, including the
Fuller-formalism, of intermediate-mass stars were calculated to make a
comparison between asteroseismically obtained core rotation rates in the core
He burning phase and in the white dwarf phase. Results: Our main results show
that models including the Fuller-formalism can match the core rotation rates
obtained for the core He burning phases. However, these models are unable to
match the rotation rates obtained for white dwarfs. When we exclude the
Fuller-formalism at the end of the core He burning phase, the white dwarf
rotation rates of the models match the observed rates. Conclusions: We conclude
that in the present form, the Fuller-formalism cannot be the sole solution for
the missing process of angular momentum transport in intermediate-mass stars.
