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The amount of $^{56}$Ni produced in type Ia supernova (SN Ia) explosion isprobably the most important physical parameter underlying the observedcorrelation of SN Ia luminosities with their light curves. Based on anempirical relation between the $^{56}$Ni mass and the light curve parameter$\triangle m_{15}$, we obtained rough estimates of the $^{56}$Ni mass for alarge sample of nearby SNe Ia with the aim of exploring the diversity in SN Ia.We found that the derived $^{56}$Ni masses for different SNe Ia could vary by afactor of ten (e.g., $M_{\rm Ni}=0.1 - 1.3$ $M_{\odot}$), which cannot beexplained in terms of the standard Chandrasekhar-mass model (with a $^{56}$Nimass production of 0.4 -- 0.8 $M_{\odot}$). Different explosion and/orprogenitor models are clearly required for various SNe Ia, in particular, forthose extremely nickel-poor and nickel-rich producers. The nickel-rich (with$M_{\rm Ni}$ $>$ 0.8 $M_{\odot}$) SNe Ia are very luminous and may have massiveprogenitors exceeding the Chandrasekhar-mass limit since extra progenitor fuelis required to produce more $^{56}$Ni to power the light curve. This is alsoconsistent with the finding that the intrinsically bright SNe Ia prefer tooccur in stellar environments of young and massive stars. For example, 75% SNeIa in spirals have $\Delta m_{15} < 1.2$ while this ratio is only 18% in E/S0galaxies. On the other hand, the nickel-poor SNe Ia (with $M_{\rm Ni}$ $<$ 0.2$M_{\odot}$) may invoke the sub-Chandrasekhar model, as most of them were foundin early-type E/S0 galaxies dominated by the older and low-mass stellarpopulations. This indicates that SNe Ia in spiral and E/S0 galaxies haveprogenitors of different properties.

Distribution of $^{56}$Ni Yields of Type Ia Supernovae and its Implication for Progenitors