Originally Posted by Wang et al

The amount of 56Ni produced in type Ia supernova (SN Ia) explosion is probably the most important physical parameter underlying the observed correlation of SN Ia luminosities with their light curves. Based on an empirical relation between the 56Ni mass and the light curve parameter △m15, we roughly determined the 56Ni mass for a large sample of nearby SNe Ia with the aim of exploring SN Ia diversity. We found that the derived 56Ni mass for different SNe Ia could vary by a factor of ten (e.g., MNi = 0.1 − 1.3M⊙), which cannot be explained in terms of the standard Chandrasekhar-mass model (with the 56Ni mass production of 0.4 – 0.8M⊙). Different explosion and/or progenitor models are distinctly required for various SNe Ia, in particular those extremely nickel-poor and nickel-rich producers. The nickel-rich (with MNi > 0.8M⊙) SNe Ia are very luminous and may have massive progenitors exceeding the Chandrasekhar-mass limit since extra progenitor fuel is required to produce more 56Ni to power the light curves...

In summary, the wide distribution of the 56Ni mass suggests that there are probably multiple origin for SN Ia explosion and/or progenitor systems.