Relevance of tidal effects and post-merger dynamics for binary neutron star parameter estimation

Dudi, Reetika; Pannarale, F.; Dietrich, Tim; Hannam, M. D.; Bernuzzi, Sebastiano; Ohme, F.; Brügmann, Bernd

doi:10.1103/physrevd.98.084061

Cited by 63 publications

(61 citation statements)

References 141 publications

(190 reference statements)

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“…The tidal contribution is overestimated at about f ∼ 1000 Hz, and later underestimated. This oscillatory behavior has been seen before, e.g., [27,34,54], and could potentially lead to biases in the estimate of tidal effects from GW signals [35]. For both NRTidal and NRTidalv2 the growth of the tidal phase around merger is much smaller than for any other approximant, which generally reduces possible pathologies in more extreme regions of the parameters, e.g., a cancellation of the point-particle and attractive tidal phase close to merger.…”

Section: Ansatz For the Nrtidal Time-domain Phasementioning

confidence: 73%

“…The hybridization is performed as discussed in Refs. [34,35] to which we refer for further details. In addition to the BNS hybrid waveforms, we also create a hybrid between the nontidal version of the TEOBResumS model and a binary black hole waveform computed with the SpEC code [75], setup SXS:BBH:0066 of the public SXS catalog [76,77].…”

Section: Hybrid Constructionmentioning

confidence: 99%

“…However, although the analytical progress has improved the performance of post-Newtonian (PN) waveform approximants, PN models still become increasingly inaccurate towards the merger, e.g. [30][31][32][33][34][35][36].…”

Section: Introductionmentioning

confidence: 99%

“…Furthermore, the analysis presented in Ref. [34,35] showed that the original NRTidal model could potentially underestimate tidal deformabilities, leading to possible biases for future detections with larger SNRs. Therefore, to further push for the availability of a fast and accurate waveform model employable for the upcoming observing runs in the advanced detector era, after recalling the basics of NRTidal and discussing the NR simulations and hybrid waveform construction in Sec.…”

Section: Introductionmentioning

confidence: 99%

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Improving the NRTidal model for binary neutron star systems

Dietrich¹,

Samajdar²,

et al. 2019

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Accurate and fast gravitational waveform (GW) models are essential to extract information about the properties of compact binary systems that generate GWs. Building on previous work, we present an extension of the NRTidal model for binary neutron star (BNS) waveforms. The upgrades are: (i) a new closed-form expression for the tidal contribution to the GW phase which includes further analytical knowledge and is calibrated to more accurate numerical relativity data than previously available; (ii) a tidal correction to the GW amplitude; (iii) an extension of the spinsector incorporating equation-of-state-dependent finite size effects at quadrupolar and octupolar order; these appear in the spin-spin tail terms and cubic-in-spin terms, both at 3.5PN. We add the new description to the precessing binary black hole waveform model IMRPhenomPv2 to obtain a frequency-domain precessing binary neutron star model. In addition, we extend the SEOBNRv4_ROM and IMRPhenomD aligned-spin binary black hole waveform models with the improved tidal phase corrections. Focusing on the new IMRPhenomPv2_NRTidalv2 approximant, we test the model by comparing with numerical relativity waveforms as well as hybrid waveforms combining tidal effective-one-body and numerical relativity data. We also check consistency against a tidal effective-one-body model across large regions of the BNS parameter space.

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Section: Ansatz For the Nrtidal Time-domain Phasementioning

confidence: 73%

Section: Hybrid Constructionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Improving the NRTidal model for binary neutron star systems

Dietrich¹,

Samajdar²,

et al. 2019

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“…In reality, Ref. [4] argued that systematic errors are small even for a loud event like GW170817 and they are likely to remain smaller than statistical errors until we detect a signal with an SNR of about 100 [42].…”

Section: Discussionmentioning

confidence: 82%

Distinguishing Binary Neutron Star from Neutron Star–Black Hole Mergers with Gravitational Waves

Chen

Chatziioannou

2020

ApJL

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The gravitational-wave signal from the merger of two neutron stars cannot be easily differentiated from the signal produced by a comparable-mass mixed binary of a neutron star and a black hole. Indeed, both binary types can account for the gravitational-wave signal GW170817 even if its electromagnetic counterpart emission is taken into account. The existence of low-mass black holes (< 5M ) is astrophysically disfavored. However, such back holes could be of primordial origin or the outcome of interactions between neutron stars and dark matter. We propose a method to identify mixed binaries of neutron stars merging with low-mass black holes using gravitational-waves alone. This method is based on the fact that certain neutron star properties that can be measured with gravitational-waves are common or similar for all neutron stars. For example all neutron stars share the same equation of state and if the latter is hadronic, neutron stars have similar radii. If a mixed binary is misidentified as a neutron star binary, the inferred neutron star properties will be misestimated and appear as outliers in a population of low-mass binaries. We show that as few as a handful of low-mass events will allow for the identification of the type of one event at the 80% confidence level. We model the population of low-mass binaries with a hierarchical mixture model and show that we can constrain the existence of mixed binaries or measure their abundance relative to neutron star binaries to ∼ 0.1 at the 68% credible level with 100 events. This method requires neither information from the post-inspiral phase of the binary, nor an EM counterpart.

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Interpreting binary neutron star mergers: describing the binary neutron star dynamics, modelling gravitational waveforms, and analyzing detections

2021

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Gravitational waves emitted from the coalescence of neutron star binaries open a new window to probe matter and fundamental physics in unexplored, extreme regimes. To extract information about the supranuclear matter inside neutron stars and the properties of the compact binary systems, robust theoretical prescriptions are required. We give an overview about general features of the dynamics and the gravitational wave signal during the binary neutron star coalescence. We briefly describe existing analytical and numerical approaches to investigate the highly dynamical, strong-field region during the merger. We review existing waveform approximants and discuss properties and possible advantages and shortcomings of individual waveform models, and their application for real gravitational-wave data analysis.

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Relevance of tidal effects and post-merger dynamics for binary neutron star parameter estimation

Cited by 63 publications

References 141 publications

Improving the NRTidal model for binary neutron star systems

Improving the NRTidal model for binary neutron star systems

Distinguishing Binary Neutron Star from Neutron Star–Black Hole Mergers with Gravitational Waves

Interpreting binary neutron star mergers: describing the binary neutron star dynamics, modelling gravitational waveforms, and analyzing detections

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