The Possible White Dwarf-Neutron Star Connection

  title={The Possible White Dwarf-Neutron Star Connection},
  author={Ram{\'o}n Canal and Jordi L. Guti{\'e}rrez},
  journal={arXiv: Astrophysics},
The current status of the problem of whether neutron stars can form, in close binary systems, by accretion-induced collapse (AIC) of white dwarfs is examined. We find that, in principle, both initially cold C+O white dwarfs in the high-mass tail of their mass distribution in binaries and O+Ne+Mg white dwarfs can produce neutron stars. Which fractions of neutron stars in different types of binaries (or descendants from binaries) might originate from this process remains uncertain. 
Nickel-rich outflows produced by the accretion-induced collapse of white dwarfs: light curves and spectra
The accretion-induced collapse (AIC) of a white dwarf to form a neutron star can leave behind a rotationally supported disc with mass of up to ~0.1 M ⊙ . The disc is initially composed of free
Type Ia Supernovae: An Examination of Potential Progenitors and the Redshift Distribution
We examine the possibility that Type Ia supernovae (SNe Ia) are produced by white dwarfs accreting from Roche lobe filling evolved companions, under the assumption that a strong optically thick
The gravitational collapse of ONe electron-degenerate cores and white dwarfs: The role of 24 Mg and 12 C revisited
The final stages of the evolution of electron-degenerate ONe cores, resulting from carbon burning in "heavy weight" intermediate-mass stars (8 M� < M < 11 M� ) and growing in mass, either from carbon
Contraindre l'équation d'état de la matière à densité supranucléaire à partir des sursauts X des étoiles à neutrons
Cette these est consacree a l'etude des oscillations periodiques detectees lors des sursauts X des etoiles a neutrons, dans des binaires X de faible masse. Ces oscillations offrent un moyen de sonder
Low-mass bare strange stars
  • R. Xu
  • Physics, Geography
  • 2004
Life Extinctions and the Gravitational Collapse of Onemg Electron-Degenerate Objects
Supernova explosions have been considered a possible (although improbable) thread to life on Earth. In 1987, a massive star exploded in the Large Magellanic Cloud and, coinciding with the arrival of


Can C+O white dwarfs form neutron stars?
Accretion-induced collapse (AIC) of white dwarfs is often invoked as the formation mechanism of neutron stars in different types of binary systems. Necessary conditions for AIC of a C + O white dwarf
The final stages of evolution of cold, mass-accreting white dwarfs
The evolution of solid C + O white dwarf models upon mass accretion is calculated up to the point of either explosive thermonuclear ignition or gravitational collapse. It is shown that both
The collapse of white dwarfs to neutron stars
The observable consequences of an accreting white dwarf collapsing directly to a neutron star are considered. The outcome depends critically upon the nature of the wind that is driven by neutrino
Accreting white dwarf models for type I supernovae. I. Presupernova evolution and triggering mechanisms
As a plausible explosion model for a Type I supernova, the evolution of carbon-oxygen white dwarfs accreting helium in binary systems was investigated from the onset of accretion up to the point at
Final Evolution of 8–10 M⊙ Stars
In stars in the range 8–10 M⊙ carbon shell burning leads to the formation of an O+Mg+Ne degenerate core. For a central density pc ≈ 5 109 g/cm3 electron captures on the core material begin. They
a companion star. Optical obser­ vations have shown that there are two main classes of such X-ray binaries: the high-mass X-ray binaries, in which the mass donor is an 0 or B star, and the low-mass
Problems of collapse and numerical relativity
Collapse and Gravitation = the Present Situation.- Presupernova Stage.- Type II Supernovae.- The Evolution of Massive Stars.- Combined Effects of Mass Loss and Extended Mixing on the Structure and
On the Formation of O-Ne White Dwarfs in Metal-rich Close Binary Systems
The evolution of primary components of initially close binary systems has been followed assuming specific initial conditions such as to have the formation of an O-Ne white dwarf at the end of a
The outcome of explosive ignition of ONeMg cores: supernovae, neutron stars, or iron white dwarfs?
Models are used to explore the outcome of explosive ignition of ONeMg cores, which result from the evolution of stars in a mass range between 8 and 10 solar masses. Arguments are presented showing