Current models of red giant stars predict higher core rotation rates than observed. This indicates the need for an efficient mechanism of angular momentum (AM) transport. Mixed modes are proposed as a mechanism of AM transport through the interaction between the mean flow and the oscillations. This mechanism has been shown to potentially explain the seismic core rotation values. We aim to uncover the potential of mixed modes as an efficient mechanism of AM transport as a function of evolution along the RGB. To this end, we test the efficiency of this mechanism for different stellar masses and for the red clump phase.