Abstract
Applying the gravitational pair production model of particle creation to a stationary, spherically symmetric neutron star using quantum Monte Carlo equations of state allows for modeling the lifetime and evolution of the neutron star. The neutron star obeys the relativistic Tolman-Oppenheimer-Volk off hydrostatic equilibrium equation and is modeled for several quantum Monte Carlo equations of state. The resulting neutron stars agree with the literature, with maximum masses between 1.76−2.46M⊙, with the variations caused by the different equations of state. By implementing a differential equation for the lifetime of the neutron star, we find the evolution of individual neutron stars, which decrease in mass and luminosity as they evaporate. The lifetime of neutron stars are of order ∼10^69 years, with maximum lifetimes in the range (1.22−3.04)×10^69 years depending on the equation of state.
Supervisor:
Professor Øystein Elgarøy, Institute of Theoretical Astrophysics, UiO
Professor David F. Mota, Institute of Theoretical Astrophysics, UiO
Intern. assessor: Associate Professor Tiago Pereira, RoCS, Institute of Theoretical Astrophysics, UiO
Extern. assessor: Professor José Beltrán Jiménez, University of Salamanca