Ways to constrain neutron star equation of state models using
  relativistic disc lines
  Relativistic spectral lines from the accretion disc of a neutron star
low-mass X-ray binary can be modelled to infer the disc inner edge radius. A
small value of this radius tentatively implies that the disc terminates either
at the neutron star hard surface, or at the innermost stable circular orbit
(ISCO). Therefore an inferred disc inner edge radius either provides the
stellar radius, or can directly constrain stellar equation of state (EoS)
models using the theoretically computed ISCO radius for the spacetime of a
rapidly spinning neutron star. However, this procedure requires numerical
computation of stellar and ISCO radii for various EoS models and neutron star
configurations using an appropriate rapidly spinning stellar spacetime. We have
fully general relativistically calculated about 16000 stable neutron star
structures to explore and establish the above mentioned procedure, and to show
that the Kerr spacetime is inadequate for this purpose. Our work systematically
studies the methods to constrain EoS models using relativistic disc lines, and
will motivate future X-ray astronomy instruments.
