I just wanted to add some info on the implosion of stars. Chandrasekhar developed the Chandrasekhar limit, which states that any star of 1.4 solar masses or less at the time of implosion will form a white dwarf. When a star has less than 2 solar masses when it collapses, but has more than 1.4, it will form a neutron star. 1.4 solar masses is the threshhold at which electron degeneracy pressure begins to fail. Neutron degeneracy pressure, as found in a neutron star, will support masses of up to 2 solar masses. Anything more massive than that will collapse to form a black hole. But note that I say mass at the time of implosion. Throughout a stars life, it will radiate away energy and go nova one or more times, depending on its itnitial size. Once every time its core implodes due to lack of nuclear fuel and forms a new element. Once a star's core becomes iron, it will not be able to gain any more energy from collapsing.

I have to go, but when I get more time I will complete this thought on the collapse of stars.

• In continuation.... - Astrophysicist - August 8, 1998 - 17:20 UTC