Measuring Neutron-Star Radii with Gravitational-Wave Detectors

Coalescing binary neutron stars (NS) are expected to be an important source of gravitational waves (GW) detectable by laser interferometers. We present here a simple method for determining the compactness ratio [Formula presented] of NS based on the observed deviation of the GW energy spectrum from point-mass behavior at the end of inspiral. Our method is based on the properties of quasiequilibrium binary NS sequences and does not require the computation of the full GW signal [Formula presented]. Combined with the measurement of the NS masses during inspiral, the determination of [Formula presented] will allow very strong constraints to be placed on the equation of state of dense nuclear matter.