We study the properties of dense matter in neutron stars and calculate
the structure of the stars based on the Zimanyi & Moszkowski (ZM) mod
el in the relativistic mean-held theory. We also compare these results
with those based on the Boguta & Bodmer (BB) model. with a recent sat
isfactory parameter set. The two models satisfy the requirements from
the observations of the masses of binary radio pulsars, the rotation f
requencies of millisecond pulsars, the redshifts of the e(+) annihilat
ion lines of some gamma-ray bursts if they are neutron stars, and the
crustal moment of inertia of neutron stars deduced from the glitch eve
nts. Other observations may provide a way to discriminate between the
two models. We suggest that the most important observational discrimin
ant between these two models is found by observing the surface radiati
on of neutron stars, since the BE model leads to a large photon fracti
on of neutron star matter and rapid cooling of neutron stars, but the
ZM model does not.