GIANT NEUTRON NUCLEUS AND PROPERTIES OF NEUTRON STARS.

Abstract

Considering a neutron star as a giant neutron nucleus composed of neutrons only, and using the binding energy, B(A, Z) expression, calculations are done for the number of neutrons A, in the giant nucleus along with the mass M and radius R of the neutron star. Two sets of calculations have been attempted. In one case the neutron star is treated as the giant nucleus, and in the calculations terms such as Coulomb energy are neglected in the expression for B. This gives A ≃ 5x1055, M = 0.042M0, R = 4.3km. In the second set of calculations, the neutron star is assumed to be in a superfluid state, where pairs of neutrons, like Cooper pairs, define the superfluid state. Pairing energy due to neutron pairs will play a definite role in determining the value of B. In this in the limiting case when B → 0, we get A ≃ 8.28x1056, M ≃ 0.7M0, R ≃ 14Km. These values compare favorably with the corresponding values known and predicted by scientists. This in turn supports the hypothesis that a neutron star may exist in a superfluid state even at very high temperatures ≃ 106 K. It is quite possible that some other particles, hitherto unknown, and forces may exist inside the neutron star, and if they are taken into account in the value of B, values of A, M, and R could be improved and the values may be closer to the values predicted so far.