  The majority of massive stars live in binary or multiple systems and will
interact during their lifetimes, which helps to explain the observed diversity
of core-collapse supernovae. Donor stars in binary systems can lose most of
their hydrogen-rich envelopes through mass transfer, which not only affects the
surface properties, but also the core structure. However, most calculations of
the core-collapse properties of massive stars rely on single-star models. We
present a systematic study of the difference between the pre-supernova
structures of single stars and stars of the same initial mass (11 - 21\Msun)
that have been stripped due to stable post-main sequence mass transfer at solar
metallicity. We present the pre-supernova core composition with novel diagrams
that give an intuitive representation of the isotope distribution. As shown in
previous studies, at the edge of the carbon-oxygen core, the binary-stripped
star models contain an extended gradient of carbon, oxygen, and neon. This
layer originates from the receding of the convective helium core during core
helium burning in binary-stripped stars, which does not occur in single-star
models. We find that this same evolutionary phase leads to systematic
differences in the final density and nuclear energy generation profiles.
Binary-stripped star models have systematically higher total masses of carbon
at the moment of core collapse compared to single star models, which likely
results in systematically different supernova yields. In about half of our
models, the silicon-burning and oxygen-rich layers merge after core silicon
burning. We discuss the implications of our findings for the explodability,
supernova observations, and nucleosynthesis from these stars. Our models will
be publicly available and can be readily used as input for supernova
simulations. [Abridged]
