7.3. BLACK HOLES 437
it is regarded as a black hole. Hence the neutron pressure gradient is thought to be a final
defense to prevent a star from collapsing into a black hole. Thus, 3M⊙becomes a critical
mass to determine the possible formation of a black hole.
2.Interaction potential pressure.However, thanks to the strong and weak interaction po-
tentials established in (Ma and Wang,2015a,2014c), there still exist three kinds of potential
pressures given by
(7.3.15) neutron potential,quark potential,weakton potential.
These three potential pressures maintain three types of astronomical bodies:
(7.3.16)
neutron stars,
quark black holes if they exist,
weakton black holes if they exist.We are now in position to discuss these potential pressures.By the theory of elementary
particles, a neutron is made up of three quarksn=uud, andu,dquarks are made up of
three weaktons asu=w∗w 1 w 1 ,d=w∗w 1 w 2. The three levels of particles possess different
potentials distinguished by their interaction charges:
(7.3.17)
neutron charge gn= 3(
ρw
ρn) 3
gs,quark charge gq=(
ρw
ρq) 3
gs,weakton weak charge gw,whereρn,ρq,ρware the radii of neutron, quark and weakton.
Letgbe a specific charge in (7.3.17). Then by the interaction potentials obtained in
(Ma and Wang,2015a), the particle with chargeghas a repulsive force:
f=g^2
r^2.
The force acts on particle’s cross section with areaS=πr^2 , which yields the interaction
potential pressure as
(7.3.18) P=
f
S=
g^2
πr^4.
Let each ballBrwith radiusrcontain only one particle. Then the mass densityρis given by
(7.3.19) ρ=
3 m 0
4 πr^3,
wherem 0 is the particle mass. By the uncertainty relation, inBrthe particle energyε 0 is
ε 0 =h ̄
2 t