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Classical novae participate in the cycle of Galactic chemical evolution inwhich grains and metal enriched gas in their ejecta, supplementing those ofsupernovae, AGB stars, and Wolf-Rayet stars, are a source of heavy elements forthe ISM. Once in the diffuse gas, this material is mixed with the existinggases and then incorporated into young stars and planetary systems during starformation. Infrared observations have confirmed the presence of carbon, SiC,hydrocarbons, and oxygen-rich silicate grains in nova ejecta, suggesting thatsome fraction of the pre-solar grains identified in meteoritic material comefrom novae. The mean mass returned by a nova outburst to the ISM probablyexceeds ~2 x 10^{-4} Solar Masses. Using the observed nova rate of 35 per yearin our Galaxy, it follows that novae introduce more than ~7 x 10^{-3} SolarMasses per year of processed matter into the ISM. Novae are expected to be themajor source of 15N and 17O in the Galaxy and to contribute to the abundancesof other isotopes in this atomic mass range. Here, we report on how changes inthe nuclear reaction rates affect the properties of the outburst and alter thepredictions of the contributions of novae to Galactic chemical evolution. Wealso discuss the necessity of including the pep reaction in studies ofthermonuclear runaways in material accreted onto white dwarfs.

The Effects of Changes in Reaction Rates on Simulations of Nova Explosions