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Mass-Radius relations for White Dwarfs consisting of a cold Fermi gas with A/Z=2. "CM" denotes the Chandrasekhar mass limit. ... ({{Information |Description= Mass-Radius relations for White Dwarfs consisting of a cold Fermi gas with A/Z=2. "CM" denotes the Chandrasekhar mass limit. |Source= Own Work |Date= 11.04.2008...
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en.wikipedia.org/wiki/File:WhiteDwarf_mass-radius.jpg
en.wikipedia.org/wiki/File:WhiteDwarf_mass-radius.jpg
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Around 1930, S. Chandrasekhar studied astrophysical models of white dwarf stars and came to the conclusion that no white dwarf can be more massive than about 1.2 solar masses (M=1.2M_\odot). This became known as the Chandrasekhar limit. ... Chandrasekhar, S. "The Maximum Mass of Ideal White Dwarfs." Astrophys. J. 74,
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scienceworld.wolfram.com/physics/ChandrasekharLimit.htm...
scienceworld.wolfram.com/physics/ChandrasekharLimit.html
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See: Chandrasekhar Limit...
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scienceworld.wolfram.com/physics/ChandrasekharMassLimit...
scienceworld.wolfram.com/physics/ChandrasekharMassLimit.html
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Hutchinson encyclopedia article about Chandrasekhar mass limit. Chandrasekhar mass limit. Information about Chandrasekhar mass limit in the Hutchinson encyclopedia. ... (redirected from Chandrasekhar mass limit)
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encyclopedia.farlex.com/Chandrasekhar+mass+limit
encyclopedia.farlex.com/Chandrasekhar+mass+limit
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Chandrasekhar limit; Chandrasekhar mass limit; Chandrasekhar mass limit; Chandrasekhar mass limit; Chandrasekhar number; Chandrasekhar Subrahmanyan; Chandrasekhar Tiwari; Chandrasekhar, Subrahmanyan; Chandrasekhar, Subrahmanyan;
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encyclopedia.farlex.com/Chandrasekhar+limit
encyclopedia.farlex.com/Chandrasekhar+limit
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The maximum mass, approximately 1.4 solar masses above which an object has too much mass to support itself against collapse by electron degeneracy pressure. Hence, the maximum mass of a white dwarf. Named after Subramanyan Chandrasekhar, the astrophysicist who first derived the white dwarf mass limit.
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www.astro.virginia.edu/~jh8h/glossary/chandrasekhar.htm
www.astro.virginia.edu/~jh8h/glossary/chandrasekhar.htm
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The problem is that SN 2006gz seemed to be too bright. In other words, it must have gotten more mass than the Chandrasekhar limit before detonating. It also had the strongest spectral signature of unburned carbon ever seen.
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www.universetoday.com/2007/11/01/colliding-white-dwarfs...
www.universetoday.com/2007/11/01/colliding-white-dwarfs-caused-a-powerful-supernova/
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Super-Chandrasekhar-mass supernovae should occur preferentially in a young stellar population, so this may provide an explanation for the observed trend that overluminous type Ia supernovae occur only in 'young' environments5, 6. As this supernova does not obey the relations that allow type Ia supernovae to be...
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www.nature.com/nature/journal/v443/n7109/abs/nature0510...
www.nature.com/nature/journal/v443/n7109/abs/nature05103.html
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The physics of the mass limit is similar to the Chandrasekhar's mass limit for compact objects, such as white dwarfs and neutron stars. ... The physics of this mass limit is very similar to the Chandrasekhar's mass limit for compact objects, such as white dwarfs and neutron stars [18]-[20]. In the dust equilibria near the...
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www.iop.org/EJ/article/1367-2630/8/1/002/njp6_1_002.htm...
www.iop.org/EJ/article/1367-2630/8/1/002/njp6_1_002.html
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