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We investigate properties of carbon-oxygen white dwarfs with respect to thecomposite uncertainties in the reaction rates using the stellar evolutiontoolkit, Modules for Experiments in Stellar Astrophysics (MESA) and theprobability density functions in the reaction rate library STARLIB. These arethe first Monte Carlo stellar evolution studies that use complete stellarmodels. Focusing on 3 M$_{\odot}$ models evolved from the pre main-sequence tothe first thermal pulse, we survey the remnant core mass, composition, andstructure properties as a function of 26 STARLIB reaction rates coveringhydrogen and helium burning using a Principal Component Analysis and SpearmanRank-Order Correlation. Relative to the arithmetic mean value, we find thewidth of the 95\% confidence interval to be $\Delta M_{{\rm 1TP}}$ $\approx$0.019 M$_{\odot}$ for the core mass at the first thermal pulse,$\Delta$$t_{\rm{1TP}}$ $\approx$ 12.50 Myr for the age, $\Delta \log(T_{{\rmc}}/{\rm K}) \approx$ 0.013 for the central temperature, $\Delta\log(\rho_{{\rm c}}/{\rm g \ cm}^{-3}) \approx$ 0.060 for the central density,$\Delta Y_{\rm{e,c}} \approx$ 2.6$\times$10$^{-5}$ for the central electronfraction, $\Delta X_{\rm c}(^{22}\rm{Ne}) \approx$ 5.8$\times$10$^{-4}$,$\Delta X_{\rm c}(^{12}\rm{C}) \approx$ 0.392, and $\Delta X_{\rmc}(^{16}\rm{O}) \approx$ 0.392. Uncertainties in the experimental$^{12}$C($\alpha,\gamma)^{16}\rm{O}$, triple-$\alpha$, and$^{14}$N($p,\gamma)^{15}\rm{O}$ reaction rates dominate these variations. Wealso consider a grid of 1 to 6 M$_{\odot}$ models evolved from the premain-sequence to the final white dwarf to probe the sensitivity of theinitial-final mass relation to experimental uncertainties in the hydrogen andhelium reaction rates.

Properties of Carbon-Oxygen White Dwarfs From Monte Carlo Stellar Models