Coalescence of black hole–neutron star binaries

Kyutoku, Koutarou; Shibata, Masaru; Taniguchi, Keisuke

doi:10.1007/s41114-021-00033-4

Cited by 53 publications

(28 citation statements)

References 639 publications

(1,101 reference statements)

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“…For GW170817, they calculate that both mechanisms have efficiencies that are consistent with GRB170817, and they can therefore not distinguish between the two. Kyutoku et al (2021) argue that neutrino pair annihilation does not occur on a sufficiently long timescale to explain the observed sGRB duration. Here we thus assumed that a jet gets launched through the BZ mechanism and followed SG21 for the accretion-to-jet energy conversion efficiency (see Barbieri et al 2019 for a similar derivation).…”

Section: Grb Jetmentioning

confidence: 87%

“…A (semi-)analytical description derived from the mapping of the output of many such simulations to a variety of associated input source parameters will be a valuable tool in the inference of a single observed source. It is worth bearing in mind that the influence of the central BH engine and surrounding ejecta on the jet propagation and opening angle is still under much debate, certainly in BHNS mergers (Kyutoku et al 2021). Systematics will be a limiting factor when incorporating such descriptions too.…”

Section: Discussionmentioning

confidence: 99%

“…Abbott et al 2017). Whether BHNS mergers are also able to produce such ultra-relativistic highly collimated outflows, or jets, is not yet fully understood (see Kyutoku et al 2021 for a recent review of BHNS mergers and the expected EM emission). If the NS is tidally disrupted, more mass may be accreted in BHNS mergers than in BNS mergers, which could increase the energy budget of the jet (see Gompertz et al 2020, and references therein).…”

Section: Grb Jetmentioning

confidence: 99%

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Investigating the detection rates and inference of gravitational-wave and radio emission from black hole neutron star mergers

Boersma

Leeuwen

2022

A&A

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Context. Black hole neutron star (BHNS) mergers have recently been detected through their gravitational-wave (GW) emission. While no electromagnetic emission has yet been confidently associated with these systems, observing any such emission could provide information on, for example, the neutron star equation of state. Black hole neutron star mergers could produce electromagnetic emission as a short gamma-ray burst (sGRB) and/or an sGRB afterglow upon interaction with the circum-merger medium. Aims. We make predictions for the expected detection rates with the Square Kilometre Array Phase 1 (SKA1) of sGRB radio afterglows associated with BHNS mergers. We also investigate the benefits of a multi-messenger analysis in inferring the properties of the merging binary. Methods. We simulated a population of BHNS mergers, making use of recent stellar population synthesis results, and estimated their sGRB afterglow flux to obtain the detection rates with SKA1. We investigate how this rate depends on the GW detector sensitivity, the primary black hole spin, and the neutron star equation of state. We then performed a multi-messenger Bayesian inference study on a fiducial BHNS merger. We simulated its sGRB afterglow and GW emission as input to this study, using recent models for both, and take systematic errors into account.Results. The expected rates of a combined GW and radio detection with the current-generation GW detectors are likely low. Due to the much increased sensitivity of future GW detectors such as the Einstein Telescope, the chances of an sGRB localisation and radio detection increase substantially. The unknown distribution of the black hole spin has a big influence on the detection rates, however, and it is a large source of uncertainty. Furthermore, when placing our fiducial BHNS merger at 50 and 100 Mpc, we are able to infer both the binary source parameters and the parameters of the sGRB afterglow simultaneously if we combine the GW and radio data.The radio data provide useful extra information on the binary parameters, such as the mass ratio, but this is limited by the systematic errors involved. For our fiducial binary at 200 Mpc, it is considerably more difficult to adequately infer the parameters of the system. Conclusions. The probability of finding an sGRB afterglow of a BHNS merger is low in the near future but will rise significantly when the next-generation GW detectors come online. Combining information from GW data with radio data is crucial for characterising the jet properties. A better understanding of the systematics will further increase the amount of information on the binary parameters that can be extracted from this radio data.

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Section: Grb Jetmentioning

confidence: 87%

Section: Discussionmentioning

confidence: 99%

Section: Grb Jetmentioning

confidence: 99%

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Investigating the detection rates and inference of gravitational-wave and radio emission from black hole neutron star mergers

Boersma

Leeuwen

2022

A&A

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“…Dense matter's presence in a merging binary, as a finite size object distorted by the gravitational field of its companion, leads to more gravitational wave emission than for black hole binaries and a faster evolution towards merger [104][105][106][107][108][109][110][111]. The size of a neutron star also determines if and when it can be tidally disrupted by a black hole companion (for black hole-neutron star binaries) and when two neutron stars collide and merge (for neutron star-neutron star binaries) [112][113][114][115]. Finally, the post-merger evolution of a neutron star-neutron star binary is strongly impacted by the properties of dense matter: unknown nuclear physics determines whether the remnant collapses to a black hole, as well as the frequency of post-merger gravitational waves driven by oscillations in the remnant [116][117][118][119][120][121][122][123][124][125][126][127][128][129][130][131][132].…”

Section: Nuclear Physics and Neutron Starsmentioning

confidence: 99%

Snowmass2021 Cosmic Frontier White Paper: Numerical relativity for next-generation gravitational-wave probes of fundamental physics

Foucart¹,

Laguna²,

Lovelace³

et al. 2022

Preprint

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The next generation of gravitational-wave detectors, conceived to begin operations in the 2030s, will probe fundamental physics with exquisite sensitivity. These observations will measure the equation of state of dense nuclear matter in the most extreme environments in the universe, reveal with exquisite fidelity the nonlinear dynamics of warped spacetime, put general relativity to the strictest test, and perhaps use black holes as cosmic particle detectors. Achieving each of these goals will require a new generation of numerical relativity simulations that will run at scale on the supercomputers of the 2030s to achieve the necessary accuracy, which far exceeds the capabilities of numerical relativity and high-performance computing infrastructures available today. Contents 1 Motivation 2 Gravitational waveform modeling 3 Nuclear physics and neutron stars 4 Modeling high-precision gravitational-wave observations 5 Testing gravity in the nonlinear regime 6 Black holes as cosmic particle detectors

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“…defining the incompressibility K 0 ≡ 9ρ 2 0 d 2 E 0 (ρ)/dρ 2 | ρ=ρ 0 and skewness J 0 ≡ 27ρ 3 0 d 3 E 0 (ρ)/dρ 3 | ρ=ρ 0 of the SNM, the slope coefficient L ≡ 3ρ 0 dE sym (ρ)/dρ| ρ=ρ 0 , the curvature coefficient K sym ≡ 9ρ 2 0 d 2 E sym (ρ)/dρ 2 | ρ=ρ 0 and the skewness coefficient J sym ≡ 27ρ 3 0 d 3 E sym (ρ)/dρ 3 | ρ=ρ 0 of the symmetry energy, etc. The EOS of ANM provides an important and basic input for various applications in both nuclear physics and astrophysics [60,80,81,78,82,83,84,85,86].…”

Section: Introductionmentioning

confidence: 99%

Equation of State of Neutron-Rich Matter in $d$-Dimensions

Cai¹,

Li²

2022

Preprint

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Nuclear systems under constraints, with high degrees of symmetries and/or collectivities may be considered as moving effectively in spaces with reduced spatial dimensions. We first derive analytical expressions for the nucleon specific energy E 0 (ρ), pressure P 0 (ρ), incompressibility coefficient K 0 (ρ) and skewness coefficient J 0 (ρ) of symmetric nucleonic matter (SNM), the quadratic symmetry energy E sym (ρ), its slope parameter L(ρ) and curvature coefficient K sym (ρ) as well as the fourth-order symmetry energy E sym,4 (ρ) of neutron-rich matter in general d spatial dimensions (abbreviated as "dD") in terms of the isoscalar and isovector parts of the isospin-dependent single-nucleon potential according to the generalized Hugenholtz-Van Hove (HVH) theorem. The equation of state (EOS) of nuclear matter in dD can be linked to that in the conventional 3-dimensional (3D) space by the ǫ-expansion which is a perturbative approch successfully used previously in treating second-order phase transitions and related critical phenomena in solid state physics and more recently in studying the EOS of cold atoms. The ǫ-expansion of nuclear EOS in dD based on a reference dimension d f = d − ǫ is shown to be effective with −1 ǫ 1 starting from 1 d f 3 in comparison with the exact expressions derived using the HVH theorem. Moreover, the EOS of SNM (with/without considering its potential part) is found to be reduced (enhanced) in lower (higher) dimensions, indicating in particular that the many-nucleon system tends to be deeper bounded but saturate at higher densities in spaces with lower dimensions. The symmetry energy perturbed from its counterpart in 3D is found to strongly depend on the momentum-dependence of the nucleon isovector potential. Moreover, the specific structure of the fourth-order symmetry energy in dD is also analyzed generally, and it is found to be naturally small, confirming the parabolic approximation for the EOS of neutron-rich matter from an even wider viewpoint. The links between the EOSs in 3D and dD spaces from the ǫ-expansion provide new perspectives to the EOS of neutron-rich matter. Further studies and potential applications of these links in nuclear physics and/or astrophysics are discussed.

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Coalescence of black hole–neutron star binaries

Cited by 53 publications

References 639 publications

Investigating the detection rates and inference of gravitational-wave and radio emission from black hole neutron star mergers

Investigating the detection rates and inference of gravitational-wave and radio emission from black hole neutron star mergers

Snowmass2021 Cosmic Frontier White Paper: Numerical relativity for next-generation gravitational-wave probes of fundamental physics

Equation of State of Neutron-Rich Matter in $d$-Dimensions

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