What is the critical mass limit for maintaining white dwarf stability?
Answer
The Chandrasekhar limit (1.4 M☉)
The long-term stability of a white dwarf hinges entirely upon its total mass remaining below a specific theoretical boundary known as the Chandrasekhar limit. This critical mass is calculated to be approximately 1.4 times the mass of the Sun (1.4 M☉). As long as the remnant mass is below this value, the quantum mechanical force of electron degeneracy pressure is sufficiently strong to perfectly balance the relentless inward pull of gravity, thus maintaining hydrostatic equilibrium indefinitely and preventing further collapse.
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