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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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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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1992
White dwarf stars represent the most common endpoint of stellar evolution. In fact, about 90% of all stars will end up as white dwarfs. Their high temperatures and low luminosities imply that they are small — only about the size of the Earth (R e = 0.009R⊙). The mean radius for white dwarfs is R = 0.01 R⊙ (see the first table).
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White dwarf stars represent the most common endpoint of stellar evolution. In fact, about 90% of all stars will end up as white dwarfs. Their high temperatures and low luminosities imply that they are small — only about the size of the Earth (R e = 0.009R⊙). The mean radius for white dwarfs is R = 0.01 R⊙ (see the first table).
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Pulsar Condition in White Dwarf Stars
Nature, 1968According to the recently proposed “astronomical sandglass model” of the pulsed radio sources1 a pulsar is a neutron star at the critical mass limit for gravitational instability. Any loss of stability resulting in incipient collapse is quickly restored by the remaining nuclear resources, which, it was assumed, can still generate thermal pulses of ...
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