“Chandrasekhar limit”的概念、定义、翻译、参考文献-科学参考

Chandrasekhar limit

Physics

The maximum possible mass of a star that is prevented from collapsing under its own gravity by the degeneracy pressure of electrons (a white dwarf). For white dwarfs the Chandrasekhar mass is about 1.4 times the mass of the sun. There is an analogue of the Chandrasekhar limit for neutron stars. For neutron stars its value is less precisely known because of uncertainties regarding the equation of state of neutron matter, but it is generally taken to be in the range of 1.5 to 3 (and almost certainly no more than 5) times the mass of the sun. It is named after the Indian-born US astrophysicist Subrahmanyan Chandrasekhar (1910–95), who discovered it in 1931.

Astronomy

The maximum possible mass of a degenerate star, above which it will be unable to support itself against the inward pull of its own gravity. For a star with no hydrogen content the limit is 1.44 solar masses, which is thus the maximum possible mass for a white dwarf. A degenerate star with a mass greater than this limit would collapse under gravity to become either a neutron star or a black hole. It is named after S. Chandrasekhar.

单词	Chandrasekhar limit
释义	Chandrasekhar limit Physics The maximum possible mass of a star that is prevented from collapsing under its own gravity by the degeneracy pressure of electrons (a white dwarf). For white dwarfs the Chandrasekhar mass is about 1.4 times the mass of the sun. There is an analogue of the Chandrasekhar limit for neutron stars. For neutron stars its value is less precisely known because of uncertainties regarding the equation of state of neutron matter, but it is generally taken to be in the range of 1.5 to 3 (and almost certainly no more than 5) times the mass of the sun. It is named after the Indian-born US astrophysicist Subrahmanyan Chandrasekhar (1910–95), who discovered it in 1931. Astronomy The maximum possible mass of a degenerate star, above which it will be unable to support itself against the inward pull of its own gravity. For a star with no hydrogen content the limit is 1.44 solar masses, which is thus the maximum possible mass for a white dwarf. A degenerate star with a mass greater than this limit would collapse under gravity to become either a neutron star or a black hole. It is named after S. Chandrasekhar.
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