Maximum mass of stable magnetized highly super-Chandrasekhar white dwarfs: stable solutions with varying magnetic fields

Abstract

We address the issue of stability of recently proposed significantly super-Chandrasekhar white dwarfs. We present stable solutions of magnetostatic equilibrium models for super-Chandrasekhar white dwarfs pertaining to various magnetic field profiles. This has been obtained by self-consistently including the effects of the magnetic pressure gradient and total magnetic density in a general relativistic framework. We estimate that the maximum stable mass of magnetized white dwarfs could be more than 3 solar mass. This is very useful to explain peculiar, overluminous type Ia supernovae which do not conform to the traditional Chandrasekhar mass-limit.

10+1 pages including 4 figures and 1 table; version accepted for publication in JCAP

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• Mass-radius relation of strongly magnetized white dwarfs: nearly independent of Landau quantization
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• Anisotropic magnetized white dwarfs: Unifying under- and over-luminous peculiar and standard type Ia supernovae
• Weak-field limit of $f(R)$ gravity to unify peculiar white dwarfs
• Suppression of luminosity and mass-radius relation of highly magnetized white dwarfs
• Formation, Possible Detection and Consequences of Highly Magnetized Compact Stars
• Screening Mechanisms on White Dwarfs: Symmetron & Dilaton
• White dwarf structure in $f(R,T,L_m)$ gravity: beyond the Chandrasekhar mass limit
• Structural Implications of the Chameleon Mechanism on White Dwarfs
• Relativistic Landau quantization in non-uniform magnetic field and its applications to white dwarfs and quantum information
• On the desert between neutron star and black hole remnants