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A white dwarf is the final evolutionary state of stars whose mass is not sufficient to become a neutron star or a black hole. This applies to over 97% of the stars in our galaxy, including our own Sun. The Lifecycle of a Low-Mass Star

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The reason they don’t collapse further is , a quantum mechanical effect that prevents electrons from occupying the same state. This pressure supports the star against gravity, creating a stable, cooling ember. white dwarf pdf vk

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The stability provided by electron degeneracy pressure is not infinite. In 1930, astrophysicist Subrahmanyan Chandrasekhar calculated the maximum mass a white dwarf can possess before gravity overcomes the quantum pressure: The reason they don’t collapse further is ,

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