Investigating GW190425 with numerical-relativity simulations

Dudi, Reetika; Adhikari, Ananya; Brügmann, Bernd; Dietrich, Tim; Hayashi, Kota; Kawaguchi, Kyohei; Kiuchi, Kenta; Kyutoku, Koutarou; Shibata, Masaru; Tichy, Wolfgang

doi:10.1103/physrevd.106.084039

Cited by 9 publications

(4 citation statements)

References 70 publications

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“…As illustrated in Figure 2, based on the BSk21 EOS, the majority of Galactic double NS systems are expected to form SMNS if they were to merge. The heaviest BNS system currently observed, GW190425, is associated with a high-spin value of the remnant, as indicated by numerical-relativity simulations (Dudi et al 2022). In contrast, some lighter double NS systems are presumed to produce low-spin stable NSs.…”

Section: Resultsmentioning

confidence: 92%

Measuring Mass and Radius of the Maximum-mass Nonrotating Neutron Star

Tang,

Gao,

et al. 2023

ApJ

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The mass (M TOV) and radius (R TOV) of the maximum-mass nonrotating neutron star (NS) play a crucial role in constraining the elusive equation of state of cold dense matter and in predicting the fate of remnants from binary neutron star (BNS) mergers. In this study, we introduce a novel method to deduce these parameters by examining the mergers of second-generation (2G) black holes (BHs) with NSs. These 2G BHs are assumed to originate from supramassive neutron stars (SMNSs) formed in BNS mergers. Since the properties of the remnant BHs arising from the collapse of SMNSs follow a universal relation governed by M TOV and R TOV, we anticipate that by analyzing a series (∼100 detections) of mass and spin measurements of the 2G BHs using the third-generation ground-based gravitational-wave detectors, M TOV and R TOV can be determined with a precision of ∼0.01M ⊙ and ∼0.6 km, respectively.

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Section: Resultsmentioning

confidence: 92%

Measuring Mass and Radius of the Maximum-mass Nonrotating Neutron Star

Tang,

Gao,

et al. 2023

ApJ

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“…GW190425 has a higher total mass (3:4 M ). There was no observed electromagnetic counterpart to that signal, a relatively unsurprising result considering the large uncertainty in the location of the source and the high likelihood that such a system did not eject a significant amount of matter (Barbieri et al 2021;Raaijmakers et al 2021;Dudi et al 2021;Camilletti et al 2022). At least two NSBH mergers were observed in 2020 (Abbott et al 2021c), with more candidates also available in the latest gravitational wave catalogue (Abbott et al 2021b).…”

Section: Observables and Existing Observationsmentioning

confidence: 99%

Neutrino transport in general relativistic neutron star merger simulations

Foucart

2023

Living Rev Comput Astrophys

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Numerical simulations of neutron star–neutron star and neutron star–black hole binaries play an important role in our ability to model gravitational-wave and electromagnetic signals powered by these systems. These simulations have to take into account a wide range of physical processes including general relativity, magnetohydrodynamics, and neutrino radiation transport. The latter is particularly important in order to understand the properties of the matter ejected by many mergers, the optical/infrared signals powered by nuclear reactions in the ejecta, and the contribution of that ejecta to astrophysical nucleosynthesis. However, accurate evolutions of the neutrino transport equations that include all relevant physical processes remain beyond our current reach. In this review, I will discuss the current state of neutrino modeling in general relativistic simulations of neutron star mergers and of their post-merger remnants. I will focus on the three main types of algorithms used in simulations so far: leakage, moments, and Monte-Carlo scheme. I will review the advantages and limitations of each scheme, as well as the various neutrino–matter interactions that should be included in simulations. We will see that the quality of the treatment of neutrinos in merger simulations has greatly increased over the last decade, but also that many potentially important interactions remain difficult to take into account in simulations (pair annihilation, oscillations, inelastic scattering).

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“…Extreme mass ratios q ∼ 2 and NS rotation close to the breakup limit remain challenging to simulate as well as to obtain clean convergence in GW higher (subdominant) modes like ( , m) = (2, 1), (3,3) and (4,4). Work in these directions is ongoing [56,60,62,63]. For example, clear fourth order convergence in the subdominant (3, 2) and (4, 4) modes for q = 1 has been shown in [63].…”

Section: Example Of Nr Waveform Analysismentioning

confidence: 99%

“…The new data were computed in simulations presented in Refs. [52][53][54][55][56][57][58][59][60][61][62][63][64] and include BNS waveforms consistent with the GW events GW170817 [54,56,57,65] and GW190425 [64,66].…”

Section: Introductionmentioning

confidence: 99%

Second release of the CoRe database of binary neutron star merger waveforms

González¹,

Zappa²,

Breschi³

et al. 2022

Preprint

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We present the second data release of gravitational waveforms from binary neutron star merger simulations performed by the Computational Relativity (CoRe) collaboration. The current database consists of 254 different binary neutron star configurations and a total of 590 individual numerical-relativity simulations using various grid resolutions. The released waveform data contain the strain and the Weyl curvature multipoles up to = m = 4. They span a significant portion of the mass, mass-ratio, spin and eccentricity parameter space and include targeted configurations to the events GW170817 and GW190425. CoRe simulations are performed with 18 different equations of state, seven of which are finite temperature models, and three of which account for non-hadronic degrees of freedom. About half of the released data

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Investigating GW190425 with numerical-relativity simulations

Cited by 9 publications

References 70 publications

Measuring Mass and Radius of the Maximum-mass Nonrotating Neutron Star

Measuring Mass and Radius of the Maximum-mass Nonrotating Neutron Star

Neutrino transport in general relativistic neutron star merger simulations

Second release of the CoRe database of binary neutron star merger waveforms

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