  Thanks to the asteroseimic study of the red giant star KIC 7341231 observed
by Kepler, it has been possible to infer its radial differential rotation
profile (Deheuvels et al. 2012). This opens new ways to constrain the physical
mechanisms responsible of the angular momentum transport in stellar interiors
by directly comparing this radial rotation profile with the ones computed using
stellar evolution codes including dynamical processes. In this preliminary
work, we computed different models of KIC 7341231 with the Geneva stellar
evolution code that includes transport mechanisms due to a shellular rotation
and the associated large-scale meridional circulation and shear-induced
turbulence. Once the global parameters of the star had been established, we
modified some of the model's input parameters in order to understand their
effects on the predicted rotation profile of the modeled star. As a result, we
find a discrepancy between the rotation profile deduced from asteroseismic
measurements and the profiles predicted from models including shellular
rotation and related meridional flows and turbulence. This indicates that a
most powerful mechanism is in action to extract angular momentum from the core
of this star.
