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Based mostly on stellar models which do not include rotation, CO white dwarfswhich accrete helium at rates of about $\sim10^{-8}~\mathrm{M}_\odot/\mathrm{yr}$ have been put forward as candidateprogenitors for a number of transient astrophysical phenomena, includingsupernovae of Type Ia, and the peculiar and fainter Type Iax supernovae. Herewe study the impact of accretion-induced spin-up including the subsequentmagnetic field generation, angular momentum transport, and viscous heating onthe white dwarf evolution up to the point of helium ignition. We resolve thestructure of the helium accreting white dwarf models with a one dimensionalLangrangian hydrodynamic code, modified to include rotational and magneticeffects. We find magnetic angular momentum transport, which leads to quasisolid-body rotation, profoundly impacts the evolution of the white dwarfmodels. Our rotating lower mass ($0.54$ and $0.82~\mathrm{M}_\odot$) modelsaccrete up to 50\% more mass up to ignition compared to the non-rotating caseand the opposite for our more massive models. Furthermore, we find thatrotation leads to up to 10-times smaller helium ignition densities, except forthe lowest adopted initial white dwarf mass. Ignition densities of order$10^6\,\mathrm{g/cm}^3$ are only found for the lowest accretion rates and forlarge amounts of accreted helium $\gtrsim 0.4\,\mathrm{M}_\odot$. However,correspondingly massive donor stars would transfer mass at much higher rates.We expect explosive He-shell burning to mostly occur as deflagrations and at$\dot{M}>2\cdot10^{-8}~\mathrm{M}_\odot/\mathrm{yr}$, regardless of white dwarfmass. Our results imply that helium accretion onto CO white dwarfs at theconsidered rates is unlikely to lead to explosions of the CO core or toclassical Type,Ia supernovae, but may instead produce events like faint andfast hydrogen-free supernovae.

Helium ignition in rotating magnetized CO white dwarfs leading to fast and faint rather than classical type Ia supernovae