Abstract
Gravitational waves from neutron star binary inspirals contain information on strongly-interacting matter in unexplored, extreme regimes. Extracting this requires robust theoretical models of the signatures of matter in the gravitational-wave signals due to spin and tidal effects. In fact, spins can have a significant impact on the tidal excitation of the quasi-normal modes of a neutron star, which is not included in current state-of-the-art waveform models. We develop a simple approximate description that accounts for the Coriolis effect of spin on the tidal excitation of the neutron star's quadrupolar and octupolar fundamental quasi-normal modes and incorporate it in the SEOBNRv4T waveform model. We show that the Coriolis effect introduces only one new interaction term in an effective action in the co-rotating frame of the star, and fix the coefficient by considering the spin-induced shift in the resonance frequencies that has been computed numerically for the mode frequencies of rotating neutron stars in the literature. We investigate the impact of relativistic corrections due to the gravitational redshift and frame-dragging effects, and identify important directions where more detailed theoretical developments are needed in the future. Comparisons of our new model to numerical relativity simulations of double neutron star and neutron star-black hole binaries show improved consistency in the agreement compared to current models used in data analysis
Highlights
The gravitational waves (GWs) from inspiraling binary systems encode detailed information about the nature and internal structure of the compact objects. These signatures arise from spin and tidal effects, including dynamical tides associated with the excitation of the objects’ characteristic quasinormal modes
We show in this paper that this can lead to non-negligible dephasings with current data analysis models which neglect this effect
IV we extend the action to a binary system and derive explicit equations of motion within the post-Newtonian approximation for the orbital dynamics
Summary
The gravitational waves (GWs) from inspiraling binary systems encode detailed information about the nature and internal structure of the compact objects. We specialize to the case of f modes, which have the largest tidal couplings, and work to linear order in the rotation frequency This leads to an effective action with one as yet undetermined coefficient characterizing the Coriolis interaction between the star’s spin and its tidal spin, i.e., the angular momentum associated with the dynamical quadrupole. VI we derive a simple phenomenological model that accounts for the Coriolis effect by applying spin-dependent shifts of the f -mode frequency and tidal deformability parameter in the existing SEOBNRv4T waveform model
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