|1. As the core is compressed, heat
|2. The added heat excites the electrons,
freeing them to form an electron cloud.
|3. As this cloud grows, it generates
its own pressure to counteract the gravitational forces
independent fusion and temperature.
|4. Stars whose mass is not large
enough for gravity to overcome this "electron degenerate"
pressure (about 1.4 Solar Masses) will
|5. Since these stars no longer
compress, the fusion process will slow down and the star will
begin to cool. This is known as a "White