The chemical yields from stars are a key
ingredient in chemical evolution models. Stars with masses as low as 0.9
solar masses, which have an age less than that of our Galaxy at low
metallicity, can contribute to the chemical evolution of elements. Stars less
than about 10 solar masses experience recurrent mixing events that can
significantly change the surface composition of the envelope, with observed
enrichments in carbon, nitrogen, fluorine, and heavy elements synthesized by
the slow neutron capture process (the s-process). These stars release their
nucleosynthesis products through stellar outflows or winds, in contrast to
massive stars that explode as core collapse supernovae. In this talk I will
review stellar yields for stars up to 10 solar masses, including a brief
discussion of their uncertainties and shortcomings. I will also discuss efforts
by various groups to address these issues and provide homogeneous yields for
low and intermediate-mass stars covering a broad range of metallicities.