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White Dwarfs and Neutron Stars [PDF]
, 2004 This chapter on the physics of compact objects begins with a section on white dwarfs. It will be shown that the famous Chandrasekhar equation is just the relativistic Thomas–Fermi equation. For white dwarfs the Thomas–Fermi approximation is ideally justified. For neutron stars the general relativistic stellar structure equations are needed.
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2014
Eddington’s theory of stars was a great success. To recall, this theory was predicated on the assumption that stars are globes of ideal gas in radiative equilibrium. The spectacular agreement between many of the predictions of this theory and observations lulled astronomers into thinking that that last word on the subject had been said.
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Eddington’s theory of stars was a great success. To recall, this theory was predicated on the assumption that stars are globes of ideal gas in radiative equilibrium. The spectacular agreement between many of the predictions of this theory and observations lulled astronomers into thinking that that last word on the subject had been said.
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The Pulsating White Dwarf Stars
Publications of the Astronomical Society of the Pacific, 2008We present a summary of what is currently known about the three distinct families of isolated pulsating white dwarfs. These are the GW Vir stars (He/C/O-atmosphere stars with Teff 120,000 K), the V777 Her stars (He-atmosphere, Teff 25,000 K), and the ZZ Ceti stars (H-atmosphere, Teff 12,000 K), all showing multiperiodic luminosity variations caused by ...
G. Fontaine, P. Brassard
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The Internal Temperature of White Dwarf Stars [PDF]
Nature, 1931 IT has recently been discovered by S. Chandrasekhar,1 B. Swirles,2 and R. C. Majumdar,3 independently, that the opacity of a degenerate gas is very small compared with what would be computed for a classical gas at the same density and temperature, the ratio being an inverse power of Sommerfeld's degeneracy-criterion parameter.
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Asteroseismology of white dwarf stars
Journal of Physics: Condensed Matter, 1998An understanding of the white dwarf stars is central to much of astrophysics, from the structure and evolution of stars to the age and history of the large ensembles of stars that we call galaxies. They are of great potential interest from the standpoint of physics as well, because they offer a chance to study matter under extreme conditions not yet ...
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Neutron Stars and White Dwarfs
1972This talk reviews the structure of neutron stars and white dwarfs, and the role of solid state physics in determining their properties. The nature of the matter in neutron stars (matter essentially in its absolute ground state), and the determination of its equation of state are first discussed; this is followed by a description of the resulting ...
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2000
I briefly review the observed properties of pulsating white dwarfs. Examples of some of the applications of seismology to these stars demonstrate how they can provide useful constraints on stellar evolution theory.
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I briefly review the observed properties of pulsating white dwarfs. Examples of some of the applications of seismology to these stars demonstrate how they can provide useful constraints on stellar evolution theory.
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2008
White dwarf stars are the burnt out remnants that remain after a star like the Sun has completed its nuclear evolution. In such a star there are no remaining nuclear energy sources, so the star evolves by simply radiating its stored thermal energy out into space.
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White dwarf stars are the burnt out remnants that remain after a star like the Sun has completed its nuclear evolution. In such a star there are no remaining nuclear energy sources, so the star evolves by simply radiating its stored thermal energy out into space.
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White dwarfs and degenerate stars
Vistas in Astronomy, 1956Abstract The observational data now known about the white dwarfs have been reviewed and analysed with special emphasis on the relationship between colour—or spectral class—and luminosity. It is found that the white dwarfs occupy a broad band, roughly parallel to, but lying about ten magnitudes below the main sequence in the H-R diagram.
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