The evolution of iron‐core white dwarfs

@article{Panei1999TheEO,
  title={The evolution of iron‐core white dwarfs},
  author={Jorge A. Panei and Leandro G. Althaus and Omar Gustavo Benvenuto},
  journal={Monthly Notices of the Royal Astronomical Society},
  year={1999},
  volume={312},
  pages={531-539}
}
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 aimed at exploring the structure and evolution of iron-core WDs by means of a detailed and updated evolutionary code. In particular, we examined the evolution of the central conditions, neutrino luminosity, surface gravity, crystallization, internal luminosity profile and ages. We find that the… Expand
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References

SHOWING 1-10 OF 24 REFERENCES
The Cooling of CO White Dwarfs: Influence of the Internal Chemical Distribution
White dwarfs are the remnants of stars of low and intermediate masses on the main sequence. Since they have exhausted all of their nuclear fuel, their evolution is just a gravothermal process. TheExpand
The fastest evolving white dwarfs
The evolution of white dwarfs (WDs) at their lowest luminosities is investigated by computing a reference track with solar metal and helium abundances down to the beginning of WD evolution. The mainExpand
Evolution of Helium White Dwarfs of Low and Intermediate Masses
We present detailed calculations of the evolution of low-mass, helium white dwarf models with masses from M = 0.1 to M = 0.5 M? at intervals of 0.05 M? and with a metallicity of Z = 10-3. For thisExpand
Effects of Fe/C phase separation on the ages of white dwarfs
The energy release associated with the phase separation of Fe from C in a predominantly C white dwarf is calculated. The total gravitational-plus-internal energy differences between models ofExpand
The Cool White Dwarf Luminosity Function and the Age of the Galactic Disk
We present new optical and infrared data for the cool white dwarfs in the proper motion sample of Liebert, Dahn, & Monet. Stellar properties—surface chemical composition, effective temperature,Expand
Evolution of DA white dwarfs in the context of a new theory of convection
In this study we compute the structure and evolution of carbon-oxygen DA white dwarfs by means of a detailed and updated evolutionary code. We treat the energy transport by convection within theExpand
DB WHITE DWARF EVOLUTION IN THE FRAME OF THE FULL SPECTRUM TURBULENCE THEORY
We present an analysis of the evolution of carbon-oxygen DB white dwarfs (helium­ rich envelope) for a wide range of effective temperatures and luminosities. To this end, we employ a full stellarExpand
Testing the White Dwarf Mass-Radius Relation with Hipparcos*
We present the Hipparcos parallaxes and resulting radii for 10 white dwarfs in visual binaries or common proper-motion systems and 11 field white dwarfs. For bright stars, Hipparcos parallaxes haveExpand
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 showingExpand
An Introduction to the Study of Stellar Structure
EDDINGTON'S “Internal Constitution of the Stars” was published in 1926 and gives what now ranks as a classical account of his own researches and of the general state of the theory at that time. SinceExpand
...
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