White Dwarf Stars
White dwarf stars are small, dense stellar remnants that are the end stage of evolution for low to medium mass stars. They are typically composed mostly of electron-degenerate matter, with a mass comparable to that of the Sun but compressed into a much smaller volume. White dwarfs are extremely hot when they form, but gradually cool over billions of years, eventually fading into black dwarfs. These objects are stable due to the balance between the inward pull of gravity and the outward pressure exerted by electron degeneracy.