Slide 16 of 59
Notes:
Neutron stars are supported by degeneracy pressure because their internal densities are so high that classical gas formulae are inappropriate to describe conditions. The ‘pressure’ is a result of Heisenberg’s Uncertainty Principle and Fermi’s Exclusion Principle, which state that particles cannot occupy the same quantum state. The resultant mechanical momenta of the particles provides the pressure of the degenerate gas.
The surface gravity of a neutron star, g(ns) is given by the equation
= (6.67e-11 x 2e30) / (1e8) m/s^2
We are going to find the value for the magnetic induction of a neutron star by thinking of the Sun contracting with its magnetic field to form a neutron star. (Although is really not known where the magnetic field in a neutron star comes from).
