  The cosmic origin of the elements, the fundamental chemical building blocks
of the Universe, is still uncertain. Binary interactions play a key role in the
evolution of many massive stars, yet their impact on chemical yields is poorly
understood. Using the MESA stellar evolution code we predict the chemical
yields ejected in wind mass loss and the supernovae of single and
binary-stripped stars. We do this with a large 162 isotope nuclear network at
solar-metallicity. We find that binary-stripped stars are more effective
producers of the elements than single stars, due to their increased mass loss
and an increased chance to eject their envelopes during a supernova. This
increased production by binaries varies across the periodic table, with
Fluorine and Potassium being more significantly produced by binary-stripped
stars than single stars. We find that the C12/C13 could be used as an indicator
of the conservativeness of mass transfer, as C13 is preferentially ejected
during mass transfer while C12 is preferentially ejected during wind mass loss.
We identify a number of gamma-ray emitting radioactive isotopes that may be
used to help constrain progenitor and explosion models of core-collapse
supernovae with next-generation gamma-ray detectors. For single stars we find
V44 and Mn52 are strong probes of the explosion model, while for
binary-stripped stars it is Cr48. Our findings highlight that binary-stripped
stars are not equivalent to two single stars and that detailed stellar
modelling is needed to predict their final nucleosynthetic yields.
