  The detonation of a sub-Chandrasekhar-mass white dwarf (WD) has emerged as
one of the most promising Type Ia supernova (SN Ia) progenitor scenarios.
Recent studies have suggested that the rapid transfer of a very small amount of
helium from one WD to another is sufficient to ignite a helium shell detonation
that subsequently triggers a carbon core detonation, yielding a
"dynamically-driven double degenerate double detonation" SN Ia. Because the
helium shell that surrounds the core explosion is so minimal, this scenario
approaches the limiting case of a bare C/O WD detonation. Motivated by
discrepancies in previous literature and by a recent need for detailed
nucleosynthetic data, we revisit simulations of naked C/O WD detonations in
this paper. We disagree to some extent with the nucleosynthetic results of
previous work on sub-Chandrasekhar-mass bare C/O WD detonations; e.g., we find
that a median-brightness SN Ia is produced by the detonation of a 1.0 Msol WD
instead of a more massive and rarer 1.1 Msol WD. The neutron-rich
nucleosynthesis in our simulations agrees broadly with some observational
constraints, although tensions remain with others. There are also discrepancies
related to the velocities of the outer ejecta and light curve shapes, but
overall our synthetic light curves and spectra are roughly consistent with
observations. We are hopeful that future multi-dimensional simulations will
resolve these issues and further bolster the dynamically-driven double
degenerate double detonation scenario's potential to explain most SNe Ia.
