Questions about electron degenerate stellar remnants.
A white dwarf, also known as a degenerate dwarf, is a type of stellar remnant. It forms from the pressured core during the death of medium stars not capable of exerting enough gravity to overcome electron resistance. White dwarfs have masses on average of about 0.5 to 0.6 Solar Masses, although there are some exceptions. A white dwarf exerts faint luminosity, that will fade over time as the light it emits are from thermal temperature which will run out over time. A white dwarf mainly contains helium with possible heavy elements such as carbon and oxygen, and a debatable coating of hydrogen. If a white draws enough mass (i.e. 1.4 solar masses) to pass the Chandrasekhar limit, fusing begins in its interior while electron resistance is overcome by gravity and the white dwarf explodes into a type Ia supernova. Once a white dwarf cools, it becomes a black dwarf. No black dwarfs exist due to the cooling time being longer than the current age of the universe.