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The majority of massive stars live in binary or multiple systems and willinteract during their lifetimes, which helps to explain the observed diversityof core-collapse supernovae. Donor stars in binary systems can lose most oftheir hydrogen-rich envelopes through mass transfer, which not only affects thesurface properties, but also the core structure. However, most calculations ofthe core-collapse properties of massive stars rely on single-star models. Wepresent a systematic study of the difference between the pre-supernovastructures 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 solarmetallicity. We present the pre-supernova core composition with novel diagramsthat give an intuitive representation of the isotope distribution. As shown inprevious studies, at the edge of the carbon-oxygen core, the binary-strippedstar models contain an extended gradient of carbon, oxygen, and neon. Thislayer originates from the receding of the convective helium core during corehelium burning in binary-stripped stars, which does not occur in single-starmodels. We find that this same evolutionary phase leads to systematicdifferences in the final density and nuclear energy generation profiles.Binary-stripped star models have systematically higher total masses of carbonat the moment of core collapse compared to single star models, which likelyresults in systematically different supernova yields. In about half of ourmodels, the silicon-burning and oxygen-rich layers merge after core siliconburning. We discuss the implications of our findings for the explodability,supernova observations, and nucleosynthesis from these stars. Our models willbe publicly available and can be readily used as input for supernovasimulations. [Abridged]

Different to the core: the pre-supernova structures of massive single and binary-stripped stars