  Fingering (thermohaline) convection has been invoked for several years as a
possible extra-mixing which could occur in Red Giant stars due to the
modification of the chemical composition induced by nuclear reactions in the
hydrogen burning zone. Recent studies show however that this mixing is not
sufficient to account for the needed surface abundances. A new prescription for
fingering convection, based on 3D numerical simulations has recently been
proposed (BGS). The resulting mixing coefficient is larger than the ones
previously given in the literature. We compute models using this new
coefficient and compare them to previous studies. We use the LPCODE stellar
evolution code with the GNA generalized version of the mixing length theory to
compute Red Giant models and we introduce fingering convection using the BGS
prescription. The results show that, although the fingering zone now reaches
the outer dynamical convective zone, the efficiency of the mixing is not enough
to account for the observations. The fingering mixing coefficient should be
increased by two orders of magnitude for the needed surface abundances to be
reached. We confirm that fingering convection cannot be the mixing process
needed to account for surface abundances in RGB stars.
