  General relativistic spectra from accretion disks around rotating neutron
stars in the appropriate space-time geometry for several different equation of
state, spin rates and mass of the compact object have been computed. The
analysis involves the computation of the relativistically corrected radial
temperature profiles and the effect of Doppler and gravitational red-shifts on
the spectra. Light bending effects have been omitted for simplicity. The
relativistic spectrum is compared with the Newtonian one and it is shown that
the difference between the two is primarily due to the different radial
temperature profile for the relativistic and Newtonian disk solutions.
  To facilitate direct comparison with observations, a simple empirical
function has been presented which describes the numerically computed
relativistic spectra well. This empirical function (which has three parameters
including normalization) also describes the Newtonian spectrum adequately. Thus
the function can in principle be used to distinguish between the two. In
particular, the best fit value of one of the parameters ($\beta$-parameter)
$\approx 0.4$ for the Newtonian case, while it ranges from 0.1 to 0.35 for
relativistic case depending upon the inclination angle, EOS, spin rate and mass
of the neutron star. Constraining this parameter by fits to future
observational data of X-ray binaries will indicate the effect of strong gravity
in the observed spectrum.
