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Over the past decades, many explosion scenarios for Type Ia supernovae havebeen proposed and investigated including various combinations of deflagrationsand detonations in white dwarfs of different masses up to the Chandrasekharmass. One of these is the gravitationally confined detonation model. In thiscase a weak deflagration burns to the surface, wraps around the bound core, andcollides at the antipode. A subsequent detonation is then initiated in thecollision area. Since the parameter space for this scenario, that is, varyingcentral densities and ignition geometries, has not been studied in detail, weused pure deflagration models of a previous parameter study dedicated to TypeIax supernovae as initial models to investigate the gravitationally confineddetonation scenario. We aim to judge whether this channel can account for oneof the many subgroups of Type Ia supernovae, or even normal events. To thisend, we employed a comprehensive pipeline for three-dimensional Type Iasupernova modeling that consists of hydrodynamic explosion simulations, nuclearnetwork calculations, and radiative transfer. The observables extracted fromthe radiative transfer are then compared to observed light curves and spectra.The study produces a wide range in masses of synthesized 56 Ni ranging from0.257 to 1.057 $M_\odot$ , and, thus, can potentially account for subluminousas well as overluminous Type Ia supernovae in terms of brightness. However, arough agreement with observed light curves and spectra can only be found for91T-like objects. Although several discrepancies remain, we conclude that thegravitationally confined detonation model cannot be ruled out as a mechanism toproduce 91T-like objects. However, the models do not provide a good explanationfor either normal Type Ia supernovae or Type Iax supernovae.

Models of pulsationally assisted gravitationally confined detonations with different ignition conditions