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Effects of neutron-star dynamic tides on gravitational waveforms within the effective-one-body approach

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Hinderer,  Tanja
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Taracchini,  Andrea
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Buonanno,  Alessandra
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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Steinhoff,  Jan
Astrophysical and Cosmological Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society;

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1602.00599.pdf
(Preprint), 481KB

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Citation

Hinderer, T., Taracchini, A., Foucart, F., Buonanno, A., Steinhoff, J., Duez, M., et al. (2016). Effects of neutron-star dynamic tides on gravitational waveforms within the effective-one-body approach. Physical Review Letters, 116: 181101. doi:10.1103/PhysRevLett.116.181101.


Cite as: https://hdl.handle.net/11858/00-001M-0000-002A-0BC7-5
Abstract
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.