# Time evolution of rotating and magnetized white dwarf stars

## TL;DR

This paper models the evolution of rotating, magnetized white dwarfs considering thermal, nuclear, and magnetic effects, estimating their lifetimes before supernova or collapse, and analyzing how magnetic braking influences their parameters.

## Contribution

It provides a comprehensive analysis of white dwarf evolution including magnetic fields, rotation, and thermal processes, offering new insights into their lifetimes and end states.

## Key findings

- Magnetic fields slow down white dwarfs without altering their structure.
- White dwarf lifetimes are estimated before supernova or collapse.
- Key parameters like temperature and angular momentum evolve predictably over time.

## Abstract

We investigate the evolution of isolated, zero and finite temperature, massive, uniformly rotating and highly magnetized white dwarf stars under angular momentum loss driven by magnetic dipole braking. We consider the structure and thermal evolution of white dwarf isothermal cores taking also into account the nuclear burning and neutrino emission processes. We estimate the white dwarf lifetime before it reaches the condition either for a type Ia supernova explosion or for the gravitational collapse to a neutron star. We study white dwarfs with surface magnetic fields from $10^6$ to $10^{9}$~G and masses from $1.39$ to $1.46~M_\odot$ and analyze the behavior of the white dwarf parameters such as moment of inertia, angular momentum, central temperature and magnetic field intensity as a function of lifetime. The magnetic field is involved only to slow down white dwarfs, without affecting their equation of state and structure. In addition, we compute the characteristic time of nuclear reactions and dynamical time scale. The astrophysical consequences of the results are discussed.