  Is the Chandrasekhar mass limit for white dwarfs (WDs) set in stone? Not
anymore -- recent observations of over-luminous, peculiar type Ia supernovae
can be explained if significantly super-Chandrasekhar WDs exist as their
progenitors, thus barring them to be used as cosmic distance indicators.
However, there is no estimate of a mass limit for these super-Chandrasekhar WD
candidates yet. Can they be arbitrarily large? In fact, the answer is no! We
arrive at this revelation by exploiting the flux freezing theorem in observed,
accreting, magnetized WDs, which brings in Landau quantization of the
underlying electron degenerate gas. This essay presents the calculations which
pave the way for the ultimate (significantly super-Chandrasekhar) mass limit of
WDs, heralding a paradigm shift 80 years after Chandrasekhar's discovery.
