Constraining the neutron star equation of state with gravitational wave signals from coalescing binary neutron stars

Agathos, M.; Meidam, J.; Pozzo, W. Del; Li, T. G. F.; Tompitak, Marco; Veitch, J.; Vitale, Salvatore; Broeck, C. Van Den

doi:10.1103/physrevd.92.023012

Cited by 203 publications

(254 citation statements)

References 87 publications

(203 reference statements)

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“…Moreover, these spectroscopic measurements will be independently checked in the near future by, e.g., waveform modeling with NICER (Gendreau et al 2012). The forthcoming measurement of the moment of inertia, which is a higher-order moment of the mass distribution of the star (Lyne et al 2004;Kramer & Wex 2009), and the prospect of eventual measurements of other higher-order moments using gravitational wave observations from coalescing neutron stars (e.g., Read et al 2009b;Del Pozzo et al 2013;Agathos et al 2015) will provide additional constraints. Finally, the recent mass measurements of approximately two-solar-mass neutron stars (Demorest et al 2010;Antoniadis et al 2013) already place strong priors on empirically inferred EOS.…”

Section: Discussionmentioning

confidence: 99%

From Neutron Star Observables to the Equation of State. I. An Optimal Parametrization

Raithel

Özel

Psaltis

2016

ApJ

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The increasing number and precision of measurements of neutron star masses, radii, and, in the near future, moments of inertia offer the possibility of precisely determining the neutron star equation of state (EOS). One way to facilitate the mapping of observables to the EOS is through a parametrization of the latter. We present here a generic method for optimizing the parametrization of any physically allowed EOS. We use mock EOS that incorporate physically diverse and extreme behavior to test how well our parametrization reproduces the global properties of the stars, by minimizing the errors in the observables of mass, radius, and the moment of inertia. We find that using piecewise polytropes and sampling the EOS with five fiducial densities between ∼1-8 times the nuclear saturation density results in optimal errors for the smallest number of parameters. Specifically, it recreates the radii of the assumed EOS to within less than 0.5 km for the extreme mock EOS and to within less than 0.12 km for 95% of a sample of 42 proposed, physically motivated EOS. Such a parametrization is also able to reproduce the maximum mass to within 0.04  M and the moment of inertia of a 1.338  M neutron star to within less than 10% for 95% of the proposed sample of EOS.

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Section: Discussionmentioning

confidence: 99%

From Neutron Star Observables to the Equation of State. I. An Optimal Parametrization

Raithel

Özel

Psaltis

2016

ApJ

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“…While the study of electromagnetic radiation from the surface of neutron stars already yields information on the state of high density matter inside [4][5][6][7][8][9][10][11], gravitational waveforms arising from quadrupolar deformations of the neutron star due to tidal effects, vibrations, rotation or elastic strain in the crust can provide additional constraints [12,13]. With current sensitivities, detectable signals come from transient but violent events such as the merger and ringdown of colliding neutron star and black hole binaries [14,15].…”

Section: Introductionmentioning

confidence: 99%

Nonradial oscillation modes of compact stars with a crust

2017

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Oscillation modes of isolated compact stars can, in principle, be a fingerprint of the equation of state (EoS) of dense matter. We study the non-radial high-frequency l=2 spheroidal modes of neutron stars and strange quark stars, adopting a two-component model (core and crust) for these two types of stars. Using perturbed fluid equations in the relativistic Cowling approximation, we explore the effect of a strangelet or hadronic crust on the oscillation modes of strange stars. The results differ from the case of neutron stars with a crust. In comparison to fluid-only configurations, we find that a solid crust on top of a neutron star increases the p-mode frequency slightly with little effect on the f -mode frequency, whereas for strange stars, a strangelet crust on top of a quark core significantly increases the f -mode frequency with little effect on the p-mode frequency.

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“…Such an analysis was used to propose a test of general relativity in [44], to probe the BH no-hair property in [45] and to explore EOS properties in [46]. We have shown that this method can significantly boost the statistical chance of detection (shown in Fig.…”

Section: Discussionmentioning

confidence: 99%

“…Apart from power stacking that simply multiplies the Bayes factor of each event [44][45][46], 1 we also investigate combining signals if the phase of the postmerger modes can be predicted using simulations informed by source parameters measured from the inspiral waveform. This is reasonable to expect by the era of third-generation gravitational wave observatories, as future numerical modeling of binary neutron star mergers is anticipated to become sufficiently accurate by then.…”

Section: A Executive Summarymentioning

confidence: 99%

Gravitational wave spectroscopy of binary neutron star merger remnants with mode stacking

et al. 2018

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A binary neutron star coalescence event has recently been observed for the first time in gravitational waves, and many more detections are expected once current ground-based detectors begin operating at design sensitivity. As in the case of binary black holes, gravitational waves generated by binary neutron stars consist of inspiral, merger, and postmerger components. Detecting the latter is important because it encodes information about the nuclear equation of state in a regime that cannot be probed prior to merger. The postmerger signal, however, can only be expected to be measurable by current detectors for events closer than roughly ten megaparsecs, which given merger rate estimates implies a low probability of observation within the expected lifetime of these detectors. We carry out Monte Carlo simulations showing that the dominant postmerger signal (the l ¼ m ¼ 2 mode) from individual binary neutron star mergers may not have a good chance of observation even with the most sensitive future ground-based gravitational wave detectors proposed so far (the Einstein Telescope and Cosmic Explorer, for certain equations of state, assuming a full year of operation, the latest merger rates, and a detection threshold corresponding to a signal-to-noise ratio of 5). For this reason, we propose two methods that stack the postmerger signal from multiple binary neutron star observations to boost the postmerger detection probability. The first method follows a commonly used practice of multiplying the Bayes factors of individual events. The second method relies on an assumption that the mode phase can be determined from the inspiral waveform, so that coherent mode stacking of the data from different events becomes possible. We find that both methods significantly improve the chances of detecting the dominant postmerger signal, making a detection very likely after a year of observation with Cosmic Explorer for certain equations of state. We also show that in terms of detection, coherent stacking is more efficient in accumulating confidence for the presence of postmerger oscillations in a signal than the first method. Moreover, assuming the postmerger signal is detected with Cosmic Explorer via stacking, we estimate through a Fisher analysis that the peak frequency can be measured to a statistical error of ∼4-20 Hz for certain equations of state. Such an error corresponds to a neutron star radius measurement to within ∼15-56 m, a fractional relative error ∼4%, suggesting that systematic errors from theoretical modeling ð≳100 m) may dominate the error budget.

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Constraining the neutron star equation of state with gravitational wave signals from coalescing binary neutron stars

Cited by 203 publications

References 87 publications

From Neutron Star Observables to the Equation of State. I. An Optimal Parametrization

From Neutron Star Observables to the Equation of State. I. An Optimal Parametrization

Nonradial oscillation modes of compact stars with a crust

Gravitational wave spectroscopy of binary neutron star merger remnants with mode stacking

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