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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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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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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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2016
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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2009
White dwarfs are the most common end-product of stellarevolution, and as such contain valuable information about the evolutionof individual stars as well as about the star formation history andsubsequent evolution in our Galaxy. In this lecture, I describe the main structural and evolutive properties of white dwarfs.
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White dwarfs are the most common end-product of stellarevolution, and as such contain valuable information about the evolutionof individual stars as well as about the star formation history andsubsequent evolution in our Galaxy. In this lecture, I describe the main structural and evolutive properties of white dwarfs.
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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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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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White Dwarfs and Neutron Stars
2004This 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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