The Chandrasekhar Mass is a fundamental limit in astrophysics that defines the maximum mass of a stable white dwarf star. It is derived from the principles of quantum mechanics and thermodynamics, particularly using the concept of electron degeneracy pressure, which arises from the Pauli exclusion principle. As a star exhausts its nuclear fuel, it collapses under gravity, and if its mass is below approximately (solar masses), the electron degeneracy pressure can counteract this collapse, allowing the star to remain stable.
The derivation includes the balance of forces where the gravitational force () acting on the star is balanced by the electron degeneracy pressure (), leading to the condition:
This relationship can be expressed mathematically, ultimately leading to the conclusion that the Chandrasekhar mass limit is given by:
where is the reduced Planck's constant, is the gravitational constant, is the mass of an electron, and $
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