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The observed sub-class of "superluminous" Type Ia supernovae lacks aconvincing theoretical explanation. If the emission of such objects werepowered exclusively by radioactive decay of 56Ni formed in the explosion, aprogenitor mass close to or even above the Chandrasekhar limit for anon-rotating white dwarf star would be required. Masses significantly exceedingthis limit can be supported by differential rotation. We, therefore, exploreexplosions and predict observables for various scenarios resulting fromdifferentially rotating carbon-oxygen white dwarfs close to their respectivelimit of stability. Specifically, we have investigated a prompt detonationmodel, detonations following an initial deflagration phase ("delayeddetonation" models), and a pure deflagration model. In postprocessing steps, weperformed nucleosynthesis and three-dimensional radiative transfercalculations, that allow us, for the first time, to consistently derivesynthetic observables from our models. We find that all explosion scenariosinvolving detonations produce very bright events. The observables predicted forthem, however, are inconsistent with any known subclass of Type Ia supernovae.Pure deflagrations resemble 2002cx-like supernovae and may contribute to thisclass. We discuss implications of our findings for the explosion mechanism andfor the existence of differentially rotating white dwarfs as supernovaprogenitors.

Thermonuclear explosions of rapidly differentially rotating white dwarfs: Candidates for superluminous Type Ia supernovae?