Distinguishing double neutron star from neutron star-black hole binary populations with gravitational wave observations

Fasano, Margherita; Wong, Kaze W. K.; Maselli, Andrea; Berti, Emanuele; Ferrari, Valeria; Sathyaprakash, B. S.

doi:10.1103/physrevd.102.023025

Cited by 27 publications

(18 citation statements)

References 130 publications

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“…We find that the tidal deformabilities are uninformative relative to a uniform prior in Λ 2 ä [0, 5000]. This measurement cannot establish the presence of NSs, which is expected given the mass ratios and S/N of the detections (Foucart et al 2013;Kumar et al 2017;Fasano et al 2020;Huang et al 2020).…”

Section: Tidal Deformability and Tidal Disruptionmentioning

confidence: 85%

Observation of Gravitational Waves from Two Neutron Star–Black Hole Coalescences

Abbott

Abraham

et al. 2021

ApJL

649

334

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We report the observation of gravitational waves from two compact binary coalescences in LIGO's and Virgo's third observing run with properties consistent with neutron star-black hole (NSBH) binaries. The two events are named GW200105_162426 and GW200115_042309, abbreviated as GW200105 and GW200115; the first was observed by LIGO Livingston and Virgo and the second by all three LIGO-Virgo detectors. The source of GW200105 has component masses -+ 8.9 1.5 1.2 and 130 Gpc yr 69 112 3 1 under the assumption of a broader distribution of component masses.

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Section: Tidal Deformability and Tidal Disruptionmentioning

confidence: 85%

Observation of Gravitational Waves from Two Neutron Star–Black Hole Coalescences

Abbott

Abraham

et al. 2021

ApJL

649

334

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“…Moreover, if the secondary object of GW190814 was a NS, it would have been swallowed by the ∼ 23M BH. Again, if the small mass component of the GW190814 event was a NS, no electromagnetic or r-process ejecta would have be observed because the tidal forces would be small [51]. In the same scenario, simulations indicate that the disk mass would be small, so the electromagnetic processes would have been difficult to detect [51,[72][73][74].…”

Section: The Strange Star Perspective: Is It Possible or Probable Acc...mentioning

confidence: 97%

“…More importantly: Is there a gap between maximum NS mass and lowest BH mass, or can they be continuously found even in the mass gap region M ∼ 2.5 − 5M [50]? In the literature, some ways for discriminating NS and BH are given [51]. These criteria are based on gravitational waves tidal deformability measurements.…”

Section: Causal Limit Of Maximum Neutron Star Mass In Jordan Frame F ...mentioning

confidence: 99%

Causal Limit of Neutron Star Maximum Mass in $f(R)$ Gravity in View of GW190814

Astashenok,

Capozziello,

Odintsov

et al. 2021

Preprint

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We investigate the causal limit of maximum mass for stars in the framework of f (R) gravity. We choose a causal equation of state, with variable speed of sound, and with the transition density and pressure corresponding to the SLy equation of state. The transition density is chosen to be equal to twice the saturation density ρt ∼ 2ρ0, and also the analysis is performed for the transition density, chosen to be equal to the saturation density ρt ∼ ρ0. We examine numerically the combined effect of the stiff causal equation of state and of the sound speed on the maximum mass of static neutron stars, in the context of Jordan frame of f (R) gravity. This yields the most extreme upper bound for neutron star masses in the context of extended gravity. As we will evince for the case of R 2 model, the upper causal mass limit lies within, but not deeply in, the mass-gap region, and is marginally the same with the general relativistic causal maximum mass, indicating that the ∼ 3M general relativistic limit is respected. In view of the modified gravity perspective for the secondary component of the GW190814 event, we also discuss the strange star possibility. Using several well established facts for neutron star physics and the Occam's razor approach, although the strange star is exciting, for the moment, it remains a possibility for describing the secondary component of GW190814. We underpin the fact that the secondary component of the compact binary GW190814 is probably a neutron star, a black hole or even a rapidly rotating neutron star, but not a strange star. We also discuss, in general, the potential role of the extended gravity description for the binary merging.

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“…Recent observations of binary neutron star mergers (Abbott et al 2017c; 2020) make neutron star science low risk because there is no doubt that binary neutron stars merge frequently enough for NEMO science. The direct measurement of the effects of matter in binary neutron stars will facilitate additional science, for example, breaking degeneracies in measurements of the Hubble flow (Messenger & Read 2012;Calderón Bustillo, Dietrich, & Lasky 2020), helping to distinguish between neutron stars and black holes (e.g., Fasano et al 2020) and any potential cosmological effects on the equation of state (e.g., Haster et al 2020).…”

Section: Other Sciencementioning

confidence: 99%

Neutron Star Extreme Matter Observatory: A kilohertz-band gravitational-wave detector in the global network

Ackley

Adya

Agrawal

et al. 2020

Publ. Astron. Soc. Aust.

187

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Gravitational waves from coalescing neutron stars encode information about nuclear matter at extreme densities, inaccessible by laboratory experiments. The late inspiral is influenced by the presence of tides, which depend on the neutron star equation of state. Neutron star mergers are expected to often produce rapidly rotating remnant neutron stars that emit gravitational waves. These will provide clues to the extremely hot post-merger environment. This signature of nuclear matter in gravitational waves contains most information in the 2–4 kHz frequency band, which is outside of the most sensitive band of current detectors. We present the design concept and science case for a Neutron Star Extreme Matter Observatory (NEMO): a gravitational-wave interferometer optimised to study nuclear physics with merging neutron stars. The concept uses high-circulating laser power, quantum squeezing, and a detector topology specifically designed to achieve the high-frequency sensitivity necessary to probe nuclear matter using gravitational waves. Above 1 kHz, the proposed strain sensitivity is comparable to full third-generation detectors at a fraction of the cost. Such sensitivity changes expected event rates for detection of post-merger remnants from approximately one per few decades with two A+ detectors to a few per year and potentially allow for the first gravitational-wave observations of supernovae, isolated neutron stars, and other exotica.

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Distinguishing double neutron star from neutron star-black hole binary populations with gravitational wave observations

Cited by 27 publications

References 130 publications

Observation of Gravitational Waves from Two Neutron Star–Black Hole Coalescences

Observation of Gravitational Waves from Two Neutron Star–Black Hole Coalescences

Causal Limit of Neutron Star Maximum Mass in $f(R)$ Gravity in View of GW190814

Neutron Star Extreme Matter Observatory: A kilohertz-band gravitational-wave detector in the global network

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