Nuclear physics and stellar evolution in 3D hydrodynamic simulations

Our knowledge of stellar evolution is limited by uncertainties coming from complex multi-dimensional processes in stellar interiors, such as convection and nuclear burning. 3D hydrodynamic models can improve this knowledge by studying realistic multi-D processes, usually for a short time range (minutes or hours).  Recent advances in computing resources are starting to enable 3D models to run for longer time and  include nuclear reactions, making the simulations more realistic and allowing study of the effects of the nuclear reactions on the stellar evolution. In this talk, I will introduce the role and impact of nuclear physics on stellar models, and present results from a set of hydrodynamic simulations of a massive-star burning phase run until fuel exhaustion, including different nuclear species. I will discuss the implications for stellar evolution, nucleosynthesis, and convection theory.