Improving the NRTidal model for binary neutron star systems

Dietrich, Tim; Samajdar, A.; Khan, S.; Johnson-McDaniel, Nathan K.; Dudi, Reetika; Tichy, Wolfgang

doi:10.1103/physrevd.100.044003

Cited by 212 publications

(212 citation statements)

References 109 publications

(234 reference statements)

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“…However, efforts are underway to further reduce waveform systematics, see e.g. [111][112][113][114][115]; such improvements will be essential for realizing the potential of BNS inspirals as probes of distinct features on the QCD phase diagram, such as the study presented here.…”

Section: Discussionmentioning

confidence: 99%

Studying strong phase transitions in neutron stars with gravitational waves

2020

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The composition of neutron stars at the extreme densities reached in their cores is currently unknown. Besides nuclear matter of normal neutrons and protons, the cores of neutron stars might harbor exotic matter such as deconfined quarks. In this paper we study strong hadron-quark phase transitions in the context of gravitational wave observations of inspiraling neutron stars. We consider upcoming detections of neutron star coalescences and model the neutron star equations of state with phase transitions through the Constant-Speed-of-Sound parametrization. We use the fact that neutron star binaries with one or more hadron-quark hybrid stars can exhibit qualitatively different tidal properties than binaries with hadronic stars of the same mass, and hierarchically model the masses and tidal properties of simulated populations of binary neutron star inspiral signals. We explore the parameter space of phase transitions and discuss under which conditions future observations of binary neutron star inspirals can identify this effect and constrain its properties, in particular the threshold density at which the transition happens and the strength of the transition. We find that if the detected population of binary neutron stars contains both hadronic and hybrid stars, the onset mass and strength of a sufficiently strong phase transition can be constrained with 50-100 detections. If the detected neutron stars are exclusively hadronic or hybrid, then it is possible to place lower or upper limits on the transition density and strength.

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Section: Discussionmentioning

confidence: 99%

Studying strong phase transitions in neutron stars with gravitational waves

2020

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“…To compute the GW phase ϕðfÞ, we use the point-mass baseline SEOBNR_BBH model and apply tidal corrections from the NRTidal framework, as in Ref. [59]. As shown in Ref.…”

Section: Parameterization Of the Nsbh Waveform Modelmentioning

confidence: 99%

“…[52][53][54][55][56][57]. References [58,59] developed a flexible technique that starts from a point-mass BBH baseline waveform and applies tidal-phase modifications by fitting a Padé-resummed post-Newtonian (PN)-based ansatz to the phasing extracted from numerical-relativity (NR) simulations (henceforth, we refer to this as the NRTidal approach). These corrections have been applied to BBH baselines produced within the EOBNR framework [60] and within the inspiral-merger-ringdown phenomenological (IMRPhenom) approach [61,62].…”

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confidence: 99%

“…[68] to describe tidal disruption of the amplitude and uses the tidalphase corrections from Ref. [59].…”

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confidence: 99%

“…[67], these waveforms were used for validation and good agreement was found. The phase is computed by applying tidal corrections to the EOBNR BBH baseline [60] using the NRTidal approach, as in SEOBNR_BNS [59]. As shown in Ref.…”

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confidence: 99%

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Aligned-spin neutron-star–black-hole waveform model based on the effective-one-body approach and numerical-relativity simulations

Matas

Dietrich²,

Buonanno³

et al. 2020

Phys. Rev. D

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After the discovery of gravitational waves from binary black holes (BBHs) and binary neutron stars (BNSs) with the LIGO and Virgo detectors, neutron-star black holes (NSBHs) are the natural next class of binary systems to be observed. In this work, we develop a waveform model for aligned-spin NSBHs combining a BBH baseline waveform (available in the effective-one-body approach) with a phenomenological description of tidal effects (extracted from numerical-relativity simulations) and correcting the amplitude during the late inspiral, merger and ringdown to account for the NS tidal disruption. In particular, we calibrate the amplitude corrections using NSBH waveforms obtained with the numerical-relativity spectral Einstein code (SpEC) and the SACRA code. The model was calibrated using simulations with NS masses in the range 1.2-1.4 M ⊙ , tidal deformabilities up to 4200 (for a 1.2 M ⊙ NS), and dimensionless BH spin magnitude up to 0.9. Based on the simulations used and on checking that sensible waveforms are produced, we recommend our model to be employed with a NS mass in the range 1-3 M ⊙ , tidal deformability 0-5000, and (dimensionless) BH spin magnitude up to 0.9. We also validate our model against two new, highly accurate NSBH waveforms with BH spin 0.9 and mass ratios 3 and 4, characterized by tidal disruption, produced with SpEC, and find very good agreement. Furthermore, we compute the unfaithfulness between waveforms from NSBH, BBH, and BNS systems, finding that it will be challenging for the Advanced LIGO-Virgo detector network at design sensitivity to distinguish different source classes. We perform a Bayesian parameter-estimation analysis on a synthetic numerical-relativity signal in zero noise to study parameter biases. Finally, we reanalyze GW170817, with the hypothesis that it is a NSBH. We do not find evidence to distinguish the BNS and NSBH hypotheses; however, the posterior for the mass ratio is shifted to less equal masses under the NSBH hypothesis.

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