A white dwarf is a stellar remnant that represents the late evolutionary stage for low-to-intermediate mass stars after they have exhausted their nuclear fuel. These celestial bodies are extremely dense, supported against gravitational collapse primarily by electron degeneracy pressure. Their composition typically consists of elements like carbon and oxygen, and they cool and dim over immense timescales, eventually becoming theoretical black dwarfs. The maximum mass a white dwarf can sustain before exceeding the critical limit and undergoing collapse is a key astrophysical constraint governing stellar evolution.