This type of model requires a mode of lighting other than a gravitational instability, which forces to find a mechanism external with dwarf white to induce an overpressure able to light fusion.
A possibility suggested is a lighting by detonation in the peripheral layer of the accrété helium of the companion who would allow to be able to light thereafter a detonation of the carbon heart by compression. This type of model could explain the under-luminous supernovæ. These types of explosion are characterized by external layers of nickel and helium of great swiftness to the top of the layers of iron and nickel (Ruiz-Lapuente1993).
The arguments in its favour are abundances of progéniteurs in better agreement with the rates of Ia and a very natural explanation to account for the dispersion of the luminosities (mass of dwarf white).
However, it seems that the simulated supernovæ are too blue to the maximum with a too fast decrease after this maximum.
If these models prove to be polluted by the elements of the layer of helium and nickel, they could be excellent candidates for the under-luminous supernovæ. However, the luminosity of the supernovæ, which is directly connected to the mass of dwarf white for this type of model, predicted in this model is more gradual than than gives the observations of the dwarf populations white ones.