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

TL;DR

This paper demonstrates the existence of stable, highly magnetized super-Chandrasekhar white dwarfs with masses exceeding 3 solar masses, providing insights into peculiar supernovae beyond traditional models.

Contribution

It presents the first stable magnetostatic equilibrium models for super-Chandrasekhar white dwarfs with varying magnetic fields in a relativistic framework.

Findings

Maximum stable mass exceeds 3 solar masses.

Magnetic fields significantly influence white dwarf stability.

Results help explain overluminous type Ia supernovae.

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.