Non-explosive DWD mergers leaving NS remnants produce optical transients detectable by LSST out to 30-820 Mpc with rates 10²-10⁶ yr⁻¹ depending on log D, though survey cadence restricts reliable detections to log D = 36-40 within 240-760 Mpc at rates 10⁴-10⁵ yr⁻¹.
Time evolution of rotating and magnetized white dwarf stars
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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.
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Optical transients from non-explosive double white-dwarf mergers: the case of a central neutron star remnant
Non-explosive DWD mergers leaving NS remnants produce optical transients detectable by LSST out to 30-820 Mpc with rates 10²-10⁶ yr⁻¹ depending on log D, though survey cadence restricts reliable detections to log D = 36-40 within 240-760 Mpc at rates 10⁴-10⁵ yr⁻¹.