Time evolution of rotating and magnetized white dwarf stars. (arXiv:1812.10543v1 [astro-ph.SR])

Time evolution of rotating and magnetized white dwarf stars. (arXiv:1812.10543v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Becerra_L/0/1/0/all/0/1">Laura Becerra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boshkayev_K/0/1/0/all/0/1">Kuantay Boshkayev</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rueda_J/0/1/0/all/0/1">Jorge. A. Rueda</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ruffini_R/0/1/0/all/0/1">Remo Ruffini</a>

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 the white dwarf isothermal core 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
analyze the behavior of the WD parameters such as the central density, radius,
moment of inertia, angular momentum, angular velocity, central temperature and
magnetic field intensity as a function of lifetime. In addition, we compute the
characteristic time of nuclear reactions and dynamical time scale. The
astrophysical consequences of the results are discussed.

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