  The EOS of strongly interacting matter at densities ten to fifteen orders of
magnitude larger than the typical density of terrestrial macroscopic objects
determines a number of neutron star properties, including the pattern of
gravitational waves emitted following the excitation of nonradial oscillation
modes. This paper reviews some of the approaches employed to model neutron star
matter, as well as the prospects for obtaining new insights from the
experimental study of gravitational waves emitted by neutron stars.
