Chandrasekhar limit

American  

[shahn-druh-sey-kahr] / ˌʃɑn drəˈseɪ kɑr /

noun

Astronomy.

1. the mass limit above which a star has too much mass to become a white dwarf after gravitational collapse, approximately 1.44 solar masses.

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Chandrasekhar limit British  

noun

1. astronomy the upper limit to the mass of a white dwarf, equal to 1.44 solar masses. A star having a mass above this limit will continue to collapse to form a neutron star

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Chandrasekhar limit Scientific  

1. The maximum size of a stable white dwarf, approximately 3 × 10 ³⁰ kg (about 1.4 times the mass of the Sun). Stars with mass higher than the Chandrasekhar limit ultimately collapse under their own weight and become neutron stars or black holes. Stars with a mass below this limit are prevented from collapsing by the degeneracy pressure of their electrons.

2. See more at degeneracy pressure

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Etymology

Origin of Chandrasekhar limit

First recorded in 1975–80; named after U.S. astrophysicist Subrahmanyan Chandrasekhar ( def. ), who formulated it

Example Sentences

Above this Chandrasekhar limit a star’s gravity will pull on itself so strongly that electrons can’t stop its collapse.

From Literature

Further calculations showed that when collapsing stars are a little more massive than the Chandrasekhar limit, the pressure of the resulting neutrons—similar to the pressure of electrons—can stave off collapse for a little while; this is what happens in a neutron star.

From Literature

But then his size was bloated immensely by the false premises of "The Apprentice" and his notoriety then began to reach — let's say, for the purposes of the metaphor — the "Chandrasekhar limit," the point at which a cold star can no longer support itself.

From Salon

At that threshold, known as the Chandrasekhar limit, theorists predict the pressure inside will cause electrons and protons to fuse into neutrons, and the white dwarf will quietly collapse into a neutron star.

From Science Magazine

Just short of the Chandrasekhar limit, at about 1.4 solar masses, the density and temperature of the core shoot up.

From Science Magazine