Programme by Session

Nuclear physics plays a critical role in galactic chemical evolution. To model abundances in stars and from supernovae it is vital to understand the relevant nuclear reaction rates and nuclear properties, such as masses and decay rates.
With hundreds of nuclei involved and thousands of possible reactions, the focus of both experimental and theoretical effort is on those cases which are needed to understand observables, such as gamma- and X-ray fluxes, light curves, isotopic ratios in grains and some elemental abundances.
This review talk will outline recent progress in constraining key nuclear reaction rates
which directly impact observables. Current challenges in the field will also be
highlighted.