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White dwarf - Wikipedia
The next step depends upon the mass of the star. Stars below the Chandrasekhar limit become stable white dwarf stars, remaining that way throughout the rest of the history of the universe absent external forces. Stars above the limit can become neutron stars or black holes. [7]: 74
For a star of 1 M ☉, the resulting white dwarf is of about 0.6 M ☉, compressed into approximately the volume of the Earth. White dwarfs are stable because the inward pull of gravity is balanced by the degeneracy pressure of the star's electrons, a consequence of the Pauli exclusion principle. Electron degeneracy pressure provides a rather ...
The Blaze Star has become a white dwarf, which happens when stars have exhausted their nuclear fuels. A "zombie star" could possibly rise from the dead on Halloween night, according to space ...
Researchers have discovered a white dwarf (a dead star), with an oxygen atmosphere surrounding it -- the first of its kind. Astronomers managed to pick up the star from spectral lines: colored ...
A Type Ia supernova (read: "type one-A") is a type of supernova that occurs in binary systems (two stars orbiting one another) in which one of the stars is a white dwarf. The other star can be anything from a giant star to an even smaller white dwarf. [1]
This white dwarf started its life as a star about twice the sun's mass, living a lifespan of perhaps 1.2 billion years before entering its death throes. Many white dwarfs have a debris disk ...
White dwarfs arise from the cores of main-sequence stars and are therefore very hot when they are formed. As they cool they will redden and dim until they eventually become dark black dwarfs. White dwarfs were observed in the 19th century, but the extremely high densities and pressures they contain were not explained until the 1920s.