Stars produce energy through nuclear fusion, producing heavier
elements from lighter ones. The heat generated from these
reactions prevents gravitational collapse of the star. Over
time, the star builds up a central core which consists of
elements which the temperature at the center of the star is not
sufficient to fuse. For main-sequence stars with a mass below
approximately 8 solar masses, the mass of this core will remain
below the Chandrasekhar limit, and they will eventually lose
mass (as planetary nebulae) until only the core, which becomes a
white dwarf, remains. Stars with higher mass will develop a
degenerate core whose mass will grow until it exceeds the limit.
At this point the star will explode in a core-collapse
supernova, leaving behind either a neutron star or a black hole.
Computed values for the limit will vary depending on the
approximations used, the nuclear composition of the mass, and
the temperature. Chandrasekhar, eq. (36),, eq. (58),, eq. (43)
gives a value of Electron degeneracy press