In this paper we examine the consequences of the propagation of a slow deflagration front through a C-0 white dwarf that leads to the formation of a marginally bound remnant. This situation corresponds to the transition between the Delayed Detonation models and the Pulsating Delayed Detonation ones. The radioactive decay of the freshly formed 56Ni not only powers the light curve but also produces an ablative front that finally disrupts the star. The light curve is characterized by its low luminosity {-16.8 m)-as compared with a normal SNia- and its broad peak (~ 100 days).

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