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Massive, highly magnetized white dwarfs with fields up to $10^9$ G have beenobserved and theoretically used for the description of a variety ofastrophysical phenomena. Ultramagnetized white dwarfs with uniform interiorfields up to $10^{18}$ G, have been recently purported to obey a new maximummass limit, $M_{\rm max}\approx 2.58~M_\odot$, which largely overcomes thetraditional Chandrasekhar value, $M_{\rm Ch}\approx 1.44~M_\odot$. Such a muchlarger limit would make these astrophysical objects viable candidates for theexplanation of the superluminous population of type Ia supernovae. We show thatseveral macro and micro physical aspects such as gravitational, dynamicalstability, breaking of spherical symmetry, general relativity, inverse$\beta$-decay, and pycnonuclear fusion reactions are of most relevance for theself-consistent description of the structure and assessment of stability ofthese objects. It is shown in this work that the first family of magnetizedwhite dwarfs indeed satisfy all the criteria of stability, while theultramagnetized white dwarfs are very unlikely to exist in nature since theyviolate minimal requests of stability. Therefore, the canonical Chandrasekharmass limit of white dwarfs has to be still applied.

Dynamical instability of white dwarfs and breaking of spherical symmetry under the presence of extreme magnetic fields