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The Last Three Seconds: Packed Message delivered by Tides in Binary Neutron Star Mergers
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It is known that the leading-order tidal effects in gravitational waveforms can be quantified by tidal deformability, while higher order terms, e.g., harmonic overtones of Love number and dynamical tides, have not been well-investigated yet. The concept of a ``form factor'', which is different from while resembles the effective tidal deformability, for the tidal interactions between neutron stars in coalescing binaries is illustrated here. The form factor effectively incorporates the contribution of dynamical tides. The dependence of tidal form factor on tidal deformability, spins, and inclination angles is modeled and expressed in a closed form.
Forward citations
Cited by 2 Pith papers
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Effective-one-body model for coalescing binary neutron stars: Incorporating tidal spin and enhanced radiation from dynamical tides
A new EOB model for BNS/NSBH inspirals adds tidal-spin back-reaction and finite-frequency radiation corrections, yielding waveform phase shifts up to a few radians that previous effective Love number models miss.
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The error budget of binary neutron star merger simulations for configurations with high spin
For highly spinning (chi=0.5) binary neutron stars, evolution code choice is the largest numerical waveform error, and current analytical models disagree with numerical relativity beyond that error after the stars touch.
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