Black dwarf supernova in the far future

@article{Caplan2020BlackDS,
  title={Black dwarf supernova in the far future},
  author={Matthew E. Caplan},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={2020},
  volume={497},
  pages={4357-4362}
}
  • M. Caplan
  • Published 2020
  • Physics
  • Monthly Notices of the Royal Astronomical Society
In the far future long after star formation has ceased the universe will be populated by sparse degenerate remnants, mostly white dwarfs, though their ultimate fate is an open question. These white dwarfs will cool and freeze solid into black dwarfs while pycnonuclear fusion will slowly process their composition to iron-56. However, due to the declining electron fraction the Chandrasekhar limit of these stars will be decreasing and will eventually be below that of the most massive black dwarfs… Expand
View PDF on arXiv
1 Citations

Figures from this paper

One Citation

Citation Type

Citation Type

Scatter-free acceleration of particles by interaction with plasma shock waves in the interstellar medium
Scatter-free acceleration is investigated for a test particle thrusted by a moving magnetized cloud in the presence of the uniform interstellar magnetic field. It is found that depending on the… Expand

References

SHOWING 1-10 OF 53 REFERENCES
A dying universe: the long-term fate and evolutionof astrophysical objects
This paper outlines astrophysical issues related to the long-term fate of the universe. The authors consider the evolution of planets, stars, stellar populations, galaxies, and the universe itself… Expand
The evolution and explosion of massive stars
Like all true stars, massive stars are gravitationally confined thermonuclear reactors whose composition evolves as energy is lost to radiation and neutrinos. Unlike lower-mass stars (M≲8M⊙),… Expand
TWO MASSIVE WHITE DWARFS FROM NGC 2323 AND THE INITIAL–FINAL MASS RELATION FOR PROGENITORS OF 4–6.5 M⊙*
We observed a sample of 10 white dwarf candidates in the rich open cluster NGC 2323 (M50) with the Keck Low-Resolution Imaging Spectrometer. The spectroscopy shows eight to be DA white dwarfs, with… Expand
Core crystallization and pile-up in the cooling sequence of evolving white dwarfs
TLDR
Photometry and parallax data from the Gaia satellite provide direct observational evidence of a theoretically predicted pile-up in the cooling sequence of white dwarfs, which is associated with core crystallization, and the energy released by crystallization in strongly coupled Coulomb plasmas is described. Expand
How Massive Single Stars End Their Life
How massive stars die—what sort of explosion and remnant each produces—depends chiefly on the masses of their helium cores and hydrogen envelopes at death. For single stars, stellar winds are the… Expand
How big can a black hole grow
I show that there is a physical limit to the mass of a black hole, above which it cannot grow through luminous accretion of gas, and so cannot appear as a quasar or active galactic nucleus (AGN). The… Expand
The evolution of iron‐core white dwarfs
Recent measurements by Hipparcos present observational evidence supporting the existence of some white dwarf (WD) stars with iron-rich core composition. In connection with this, the present paper is… Expand
Do electron-capture supernovae make neutron stars? First multidimensional hydrodynamic simulations of the oxygen deflagration
In the classical picture, electron-capture supernovae and the accretion-induced collapse of oxygen-neon white dwarfs (ONeWDs) undergo an oxygen deflagration phase before gravitational collapse… Expand
An Empirical Measurement of the Initial-Final Mass Relation with Gaia White Dwarfs
We use data from Gaia DR2 to constrain the initial-final mass relation (IFMR) for field stars with initial masses $0.9 \lesssim m_{\rm in}/M_{\odot} \lesssim 8$. Precise parallaxes have revealed… Expand
The initial–final mass relationship of white dwarfs revisited: effect on the luminosity function and mass distribution
The initial-final mass relationship connects the mass of a white dwarf with the mass of its progenitor in the main-sequence. Although this function is of fundamental importance to several fields in… Expand
...
1
2
3
4
5
...