This section covers the nucleosynthesis in massive stars during their evolution up to the supernova phase including the elements ejected through stellar winds in the Wolf-Rayet phase. This is followed by a review on the theoretical results for the supernova yields and a discussion of the uncertainties affecting these yields. The evolution and the nucleosynthesis in intermediate mass stars are then discussed as well as those stars' contribution to the chemical enrichment of the ISM.

      Abundance analyses results are reviewed, covering very metal-poor and mildly metal-poor stars as well as globular cluster stars. The emphasis is placed on the main differences as well as on the common features.

      This section covers what can be said as to the kinematics of metal-poor stars and globular clusters. Formation scenarios of the thick disk and the halo are discussed.

      A confrontation between observed colour-magnitude diagrams and theoretical HR diagrams of globular clusters is presented. Special emphasis is put on the uncertainties affecting both the observational location of a star in a colour-magnitude diagram and on the theoretical uncertainties in the modelling of low-mass stars used in the computation of theoretical isochrones. Ages of globular clusters are also addressed.

      Early stages of globular clusters are presented with an emphasis on the possibility of self-enrichment. This is followed by a discussion on the dynamical evolution of globular clusters with special attention given to the conditions of disruption and to the evaporation of stars from a stable cluster.