Inferring the neutron star equation of state from binary inspiral waveforms
arXiv:1008.1822 · doi:10.1142/9789814374552_0046
Abstract
The properties of neutron star matter above nuclear density are not precisely known. Gravitational waves emitted from binary neutron stars during their late stages of inspiral and merger contain imprints of the neutron-star equation of state. Measuring departures from the point-particle limit of the late inspiral waveform allows one to measure properties of the equation of state via gravitational wave observations. This and a companion talk by J. S. Read reports a comparison of numerical waveforms from simulations of inspiraling neutron-star binaries, computed for equations of state with varying stiffness. We calculate the signal strength of the difference between waveforms for various commissioned and proposed interferometric gravitational wave detectors and show that observations at frequencies around 1 kHz will be able to measure a compactness parameter and constrain the possible neutron-star equations of state.
Talk given at the 12th Marcel Grossman Meeting, Paris, France, 12-18 Jul 2009
Cited by in corpus (7)
- Rotating Stars in Relativity
- Observing and measuring the neutron-star equation-of-state in spinning binary neutron star systems
- Dynamical tides in coalescing superfluid neutron star binaries with hyperon cores and their detectability with third generation gravitational-wave detectors
- Measuring neutron star tidal deformability with Advanced LIGO: a Bayesian analysis of neutron star - black hole binary observations
- Comprehensive analysis of the tidal effect in gravitational waves and implication for cosmology
- Neutron Star Crust and Molecular Dynamics Simulation
- Review of Multi-messenger observations of neutron rich matter