  Context: Asteroseismic measurements reveal that an unknown efficient angular
momentum (AM) transport mechanism is needed for subgiant and red giant stars. A
revised prescription for AM transport by the magnetic Tayler instability has
been recently proposed as a possible candidate for such a missing mechanism.
  Results: The revised prescription for the transport by the Tayler instability
leads to low core rotation rates after the main sequence that are in better
global agreement with asteroseismic measurements than those predicted by models
with purely hydrodynamic processes or with the original Tayler-Spruit dynamo. A
detailed comparison with asteroseismic data shows that the rotational
properties of at most two of the six subgiants can be correctly reproduced by
models accounting for this revised magnetic transport process. This result is
obtained independently of the value adopted for the calibration parameter in
this prescription. We also find that this transport by the Tayler instability
faces difficulties in simultaneously reproducing asteroseismic measurements
available for subgiant and red giant stars. The low values of the calibration
parameter needed to correctly reproduce the rotational properties of two of the
six subgiants lead to core rotation rates during the red giant phase that are
too high. Inversely, the higher values of this parameter needed to reproduce
the core rotation rates of red giants lead to a very low degree of radial
differential rotation before the red giant phase, which is in contradiction
with the internal rotation of subgiant stars.
  Conclusions: In its present form, the revised prescription for the transport
by the Tayler instability does not provide a complete solution to the missing
AM transport revealed by asteroseismology of evolved stars.
