  One of the largest uncertainties in stellar evolutionary computations is the
accuracy of the considered reaction rates. The 12C(alpha,gamma)16O reaction is
particularly important for the study of low- and intermediate-mass stars as it
determines the final C/O ratio in the core which influences the white dwarf
cooling evolution. Thus, there is a need for a study of how the computations of
white dwarfs and their progenitors that are made to date may be affected by the
uncertainties of the 12C(alpha,gamma)16O reaction rates. In this work we
compute fully evolutionary sequences using the MESA code with initial masses in
the range of 0.90 <= Mi/Msun <= 3.05. We consider different adopted reaction
rates, obtained from the literature, as well as the extreme limits within their
uncertainties. As expected, we find that previous to the core helium burning
stage there are no changes to the evolution of the stars. However, the
subsequent stages are all affected by the uncertainties of the considered
reaction rate. In particular, we find differences to the convective core mass
during the core helium burning stage which may affect pulsation properties of
subdwarfs, the number of thermal pulses during the asymptotic giant branch and
trends between final oxygen abundance in the core and the progenitor masses of
the remnant white dwarfs.
