Chandrasekhar limit is 1.4 solar masses
Image: Omarius257, CC BY-SA 4.0, via Wikimedia Commons
Chandrasekhar limit
Chandrasekhar limit is 1.4 solar masses
The Chandrasekhar limit is the maximum mass for a stable white dwarf star, beyond which electron degeneracy pressure cannot prevent gravitational collapse.
This limit is crucial for understanding the fate of white dwarf stars. When a white dwarf exceeds this mass, it can no longer support itself against gravitational forces, leading to potential collapse into a neutron star or black hole.
The value of the Chandrasekhar limit depends on the ratio of electrons to nucleons in the star. For small stars, this ratio is around 1/2, resulting in a limit of approximately 1.44 solar masses.
Remember this
Understanding the Chandrasekhar limit is essential for predicting the evolution and ultimate fate of white dwarf stars in the universe.
Text adapted from Wikipedia, licensed under CC BY-SA 4.0.
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