Neutron star equation of state

New observations of neutron stars from sources such as radio pulsars, X-ray binaries, quasi-periodic oscillators, X-ray bursters and thermally-emitting isolated neutron stars, can ultimately constrain the dense matter equation of state. Observable quantities include neutron star masses, radii, rotation rates, radiation radii, redshifts, moments of inertia, temperatures and ages. Several ways in which these quantities can lead to theoretical limits are discussed.