| Neutron stars are popular research tools for nuclear physicists since they are the densest observable objects in the Universe. To constrain the physics of pure neutron matter, we study the phenomenon of glitches and compare recent physical models of these glitches to pure neutron matter equations of state. Using a realistic equation of state and realistic moment of inertia equations for a slowly rotating neutron star, we can compare these results to observation data from the last half century.;It is assumed that there is a sea of superfluid neutrons in the inner layers of the neutron star that interact with the other components and give their angular momentum to the crust to allow the star to spin, or glitch. By varying the physical constraints of how the superfluid neutrons interact in the core and crust while changing how the pressure and density of the star are related, we can calculate the moment of inertia for different masses, radii, etc. Using observations, we can constrain the three previous degrees of freedom. The population distribution of neutron stars is currently unknown and can be tested using the above method but using the overall data from glitches as an average.;Using this method, we constrained the strength of interaction inside the core and in the inner crust of the neutron star. The relation between the pressure and density of the neutron star in this test has been constrained to ~≤ 60 MeV which is consistent with other independent results for other phenomena in neutron stars. |
