2016/02/29 by Tanja Hinderer, Andrea Taracchini, Francois Foucart +15 · 337 citations
Earth and Planetary Sciences · Physics and Astronomy · #Astronomy #Astrophysics #Gamma-ray bursts and supernovae #Geophysics and Gravity Measurements #Gravitation #Gravitational wave #Neutron #Neutron star #Nuclear physics #Physics #Pulsars and Gravitational Waves Research #Quantum mechanics #Waveform #astro-ph.HE #astro-ph.SR #gr-qc
paper · pdf · doi:10.1103/physrevlett.116.181101
published in Physical Review Letters 116(18), 181101 (American Physical Society)
openalex publication_date 2016/05/05 · arxiv created 2016/05/09 · arxiv updated 2016/05/11 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Extracting the unique information on ultradense nuclear matter from the gravitational waves emitted by merging neutron-star binaries requires robust theoretical models of the signal. We develop a novel effective-one-body waveform model that includes, for the first time, dynamic (instead of only adiabatic) tides of the neutron star as well as the merger signal for neutron-star-black-hole binaries. We demonstrate the importance of the dynamic tides by comparing our model against new numerical-relativity simulations of nonspinning neutron-star-black-hole binaries spanning more than 24 gravitational-wave cycles, and to other existing numerical simulations for double neutron-star systems. Furthermore, we derive an effective description that makes explicit the dependence of matter effects on two key parameters: tidal deformability and fundamental oscillation frequency.