Abstract
Tidal effects in gravitational-wave (GW) observations from binary neutron star mergers have the potential to probe ultradense matter and shed light on the unknown nuclear equation of state of neutron stars. Tidal effects in inspiralling neutron star binaries become relevant at GW frequencies of a few hundred Hz and require detectors with exquisite high-frequency sensitivity. Third generation GW detectors such as the Einstein Telescope or Cosmic Explorer will be particularly sensitive in this high-frequency regime, allowing us to probe neutron star tides beyond the adiabatic approximation. Here we assess whether dynamical tides can be measured from a neutron star inspiral. We find that the measurability of dynamical tides depends strongly on the neutron star mass and equation of state. For a semirealistic population of 10,000 inspiralling binary neutron stars, we conservatively estimate that on average 𝒪( 50 ) binaries will have measurable dynamical tides. As dynamical tides are characterized not only by the star’s tidal deformability but also by its fundamental (f-) mode frequency, they present a possibility of probing higher-order tidal effects and test consistency with quasiuniversal relations. For a GW170817-like signal in a third generation detector network, we find that the stars’ f-mode frequencies can be measured to within a few hundred Hz.
| Original language | English |
|---|---|
| Article number | 123032 |
| Number of pages | 17 |
| Journal | Physical Review D (Particles, Fields, Gravitation and Cosmology) |
| Volume | 105 |
| Issue number | 12 |
| DOIs | |
| Publication status | Published - 15 Jun 2022 |
Bibliographical note
Funding Information:We thank Jocelyn Read for useful discussions and Richard O’Shaughnessy for comments on the manuscript as well as Sam Higginbotham for his contribution to the very early stages of this project. N. W. and G. P. are supported by STFC, the School of Physics and Astronomy at the University of Birmingham and the Birmingham Institute for Gravitational Wave Astronomy. P. S. acknowledges support from STFC grant No. ST/V005677/1. Computations were performed using the University of Birmingham’s BlueBEAR HPC service, which provides a High Performance Computing service to the University’s research community, as well as resources provided by Supercomputing Wales, funded by STFC Grants No. ST/I006285/1 and No. ST/V001167/1 supporting the UK Involvement in the Operation of Advanced LIGO. Part of this research was performed while G. P. and P. S. were visiting the Institute for Pure and Applied Mathematics (IPAM), which is supported by the National Science Foundation (Grant No. DMS-1925919). This manuscript has the LIGO document number P2200030.
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© 2022 American Physical Society.