luckis11 said:
Thanks for the info. So I guess my last post is totally according to the theory. But you did not answer this question:
ΔΜ of nucleons=m-μ,
m=mass of the nucleons before the reaction,
μ=mass of the nucleons after the reaction,
u=speed of the nucleons before the reaction,
U=speed of the nucleons after the reaction,
i.e. ignoring the electrons for the moment
(m-μ)c^2=(1/2)μU^2-(1/2)mu^2, or
(m-μ)c^2=(1/2)μU^2-(1/2)mu^2+light?
I.e. the born light comes from the dissolution of electrons alone, or also from the ΔΜ of nucleons?
One is headed in the right direction, but not quite there.
Firstly, it's not the mass of the nucleons, but the nuclei. If it was 4 protons (p) combining to one alpha (
2He
4), it would be the mass of 4 protons - mass of an alpha particle (He nucleus). Proton-proton fusion, which is one of the reactions in stars, is part of a complicated chain of reactions. Four protons would never spontaneous fuse to form an alpha particle.
In the case of d+t => α+n, then one looks at the masses: (m
d + m
t - m
α - m
n)c
2 = Q. If Q > 0, i.e., the reaction is exothermic, the increase in energy manifest in the increase in kinetic energy of the products (α, n) over the kinetic energies of the reactants (d, t). The total energy is conserved, and one must also consider the conservation of momentum.
In a thermonuclear device, fission trigger produces a prodigious amount of X-rays as the electrons around the fission products reconfigure to ground states (in addition to the kinetic energy of the fission products = a lot of thermal energy = high temperature), while other electrons experience bremsstrahlung effects. The quantity of X-rays heats the fusion system, which then causes fusion of light isotopes, e.g., the aforementioned d,t, which also gets very hot. Very hot = high temperatures on the order of many keV (many millions K; 1 keV = 11.6 million K). Very hot masses produce light from the very excited electrons and as electrons recombine with nuclei (or ions). Some excited nuclei can emit gamma rays as they decay to a lower energy state.
For nuclei to undergo fusion, they have to have some initial kinetic energy so that the nuclei can approach each other in order to 'fuse', or rather, undergo the nuclear reaction. Nuclei of different masses do not necessarily have the same kinetic energy, especially if they are not in thermal equilibrium, as in the case of a very rapid transient.
In more general terms of a binary nuclear reaction:
(T + E
0)
a + (T + E
0)
b = (T + E
0)
c + (T + E
0)
d, where T is kinetic energy, E
0 is rest mass, and a,b;c,d indicate reactant nuclei (a,b) and product nuclei, or nucleon (c,d). Protons and neutrons can be products of some fusion reactions.
See pages 2, 3 and 4 of
https://www.lehigh.edu/~eus204/teaching/ME362/lectures/lecture01.pdf