  Nuclear physics can be applied in various ways to the study of neutron stars.
This thesis reports on one such application, where the relativistic mean-field
approximation has been employed to calculate the equations of state of matter
in the neutron star interior. In particular the equations of state of nuclear
and neutron star matter of the NL3, PK1 and FSUGold parameter sets were
derived. A survey of available literature on neutron stars is presented and we
use the derived equations of state to reproduce the properties of saturated
nuclear matter as well as the mass-radius relationship of a static, spherical
symmetric neutron star. Results are compared to published values of the
properties of saturated nuclear matter and to available observational data of
the mass-radius relationship of neutron stars.
