2016/03/03 by Kenta Hotokezaka, Koutarou Kyutoku, Yuichiro Sekiguchi +2 · 7 citations
Earth and Planetary Sciences · Physics and Astronomy · #Astrophysics #Dimensionless quantity #Equation of state #General relativity #Geophysics and Gravity Measurements #Gravitational wave #High-pressure geophysics and materials #LIGO #Lambda #Mathematical physics #Neutron star #Numerical relativity #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #RADIUS #Sigma #gr-qc
paper · pdf · doi:10.1103/physrevd.93.064082
18 pages, 9 figures, accepted for publication in PRD
arxiv created 2016/03/03 · openalex publication_date 2016/03/31 · arxiv updated 2016/04/20 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Combining new gravitational waveforms derived by long-term (14 to 16 orbit) numerical-relativity simulations with waveforms by an effective-one-body (EOB) formalism for coalescing binary neutron stars, we construct hybrid waveforms and estimate the measurability for the dimensionless tidal deformability of the neutron stars, \mathrm\ensuremathΛ, by advanced gravitational-wave detectors. We focus on the equal-mass case with the total mass 2.7M_\ensuremath\bigodot. We find that for an event at a hypothetical effective distance of Deff=200 Mpc, the distinguishable difference in the dimensionless tidal deformability will be \ensuremath≈100, 400, and 800 at 1\ensuremathσ, 2\ensuremathσ, and 3\ensuremathσ levels, respectively, for Advanced LIGO. If the true equation of state is stiff and the typical neutron-star radius is R\ensuremath\gtrsim13 km, our analysis suggests that the radius will be constrained within \ensuremath≈1 km at 2\ensuremathσ level for an event at Deff=200 Mpc. On the other hand, if the true equation of state is soft and the typical neutron-star radius is R\ensuremath\lesssim12 km, it will be difficult to narrow down the equation of state among many soft ones, although it is still possible to discriminate the true one from stiff equations of state with R\ensuremath\gtrsim13 km. We also find that gravitational waves from binary neutron stars will be distinguished from those from spinless binary black holes at more than 2\ensuremathσ level for an event at Deff=200 Mpc. The validity of the EOB formalism, Taylor-T4, and Taylor-F2 approximants as the inspiral waveform model is also examined.