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Chandrasekhar limit

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description Chandrasekhar limit Overview

The Chandrasekhar limit represents the critical mass a stellar remnant can sustain against gravitational collapse. It’s approximately 1.44 solar masses, established for white dwarf stars composed primarily of carbon and oxygen. This limit dictates the fate of these stars; exceeding it initiates a supernova explosion. The concept is fundamental in astrophysics and is particularly relevant to understanding the evolution and demise of massive stars and remnants like white dwarfs.

help Chandrasekhar limit FAQ

What is the Chandrasekhar limit in simple terms?

The Chandrasekhar limit is the maximum mass a white dwarf can have before electron degeneracy pressure can no longer support it. The commonly quoted value is about 1.4 times the mass of the Sun.

What happens if a white dwarf exceeds the Chandrasekhar limit?

If a white dwarf gains too much mass, it can collapse or trigger runaway nuclear burning depending on its situation. In a binary system, that process is tied to Type Ia supernova models.

Who was Subrahmanyan Chandrasekhar?

Subrahmanyan Chandrasekhar was an Indian-American astrophysicist who worked out the white-dwarf mass limit in the early 20th century. He later received the 1983 Nobel Prize in Physics, shared with William A. Fowler.

Why is the Chandrasekhar limit important for astronomy?

It helps explain why white dwarfs are stable only below a certain mass. It is also part of the physics behind Type Ia supernovae, which astronomers use as distance indicators across the universe.

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