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

The impact of the uncertainties in the 12C({\alpha},{\gamma})16O reaction rate on the evolution of low- to intermediate-mass stars