What is the relationship between neutron stars and the Chandrasekhar Limit?
The Chandrasekhar Limit is the most mass the core of a dying star can contain and still become a White Dwarf. White Dwarfs are held up against gravitational collapse by electron degeneracy pressure. Any mass more than the Chandrasekhar Limit will over power this pressure and create a Neutron Star. The pressure is so great that electrons are literally pushed into protons, creating neutrons, hence the name.
