Electron degeneracy, which is a result of the Pauli exclusion principle, is important in

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Electron degeneracy pressure becomes significant in the core of a star when the core's temperature and density are such that electrons are forced into the same energy states, as per the Pauli exclusion principle. This typically happens in the late stages of a star's life, such as just before the start of core helium burning, when the core has exhausted its hydrogen fuel and is not yet hot enough for helium fusion to begin. In this phase, the core contracts under gravity, and electron degeneracy pressure helps to support the star against further gravitational collapse.

Electron Degeneracy, Which Is a Result of the Pauli Exclusion