Type Ia supernovae ( SNeIa ) , used as one of the standard candles in astrophysics , are believed to form when the mass of the white dwarf approaches Chandrasekhar mass limit .
However , observations in last few decades detected some peculiar SNeIa , which are predicted to be originating from white dwarfs of mass much less than the Chandrasekhar mass limit or much higher than it .
Although the unification of these two sub-classes of SNeIa was attempted earlier by our group , in this work , we , for the first time , explain this phenomenon in terms of just one property of the white dwarf which is its central density .
Thereby we do not vary the fundamental parameters of the underlying gravity model in the contrary to the earlier attempt .
We effectively consider higher order corrections to the Starobinsky- f ( R ) gravity model to reveal the unification .
We show that the limiting mass of a white dwarf is \sim M _ { \odot } for central density \rho _ { c } \sim 1.4 \times 10 ^ { 8 } g/cc , while it is \sim 2.8 M _ { \odot } for \rho _ { c } \sim 1.6 \times 10 ^ { 10 } g/cc under the same model parameters .
We further confirm that these models are viable with respect to the solar system test .
This perhaps enlightens very strongly the long standing puzzle lying with the predicted variation of progenitor mass in SNeIa .