GW190814: on the properties of the secondary component of the binary

Biswas, B.; Nandi, Rana; Char, Prasanta; Bose, S.; Stergioulas, Nikolaos

doi:10.1093/mnras/stab1383

Cited by 60 publications

(57 citation statements)

References 67 publications

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“…Tidal effects are quantified through the dimensionless tidal deformability Λ, which scales roughly as ðR=mÞ 6 [26] for a NS of mass m and radius R, implying that the most massive-and thus most compact-NSs exhibit inherently weaker tidal interactions. As an result, the very nature of some ∼2-3 M ⊙ compact objects observed with GWs, such as the primary in GW190425 [27] and the secondary in GW190814 [28], cannot be determined beyond a reasonable doubt [29][30][31][32][33][34]. In the same density regime as the GWs, the electromagnetic counterpart to GW170817 may bound the EoS stiffness from below [35][36][37][38], though it is subject to significant systematic modeling uncertainty [39,40].…”

Section: Introductionmentioning

confidence: 99%

Impact of the PSR J0740+6620 radius constraint on the properties of high-density matter

et al. 2021

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X-ray pulse profile modeling of PSR J0740 þ 6620, the most massive known pulsar, with data from the NICER and XMM-Newton observatories recently led to a measurement of its radius. We investigate this measurement's implications for the neutron star equation of state (EoS), employing a nonparametric EoS model based on Gaussian processes and combining information from other x-ray, radio and gravitationalwave observations of neutron stars. Our analysis mildly disfavors EoSs that support a disconnected hybrid star branch in the mass-radius relation, a proxy for strong phase transitions, with a Bayes factor of 6.9. For such EoSs, the transition mass from the hadronic to the hybrid branch is constrained to lie outside ð1; 2Þ M ⊙ . We also find that the conformal sound-speed bound is violated inside neutron star cores, which implies that the core matter is strongly interacting. The squared sound speed reaches a maximum of 0.75 þ0.25 −0.24 c 2 at 3.60 þ2.25 −1.89 times nuclear saturation density at 90% credibility. Since all but the gravitational-wave observations prefer a relatively stiff EoS, PSR J0740 þ 6620's central density is only 3.57 þ1.3 −1.3 times nuclear saturation, limiting the density range probed by observations of cold, nonrotating neutron stars in β-equilibrium.

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Section: Introductionmentioning

confidence: 99%

Impact of the PSR J0740+6620 radius constraint on the properties of high-density matter

et al. 2021

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“…Although its nature is uncertain (e.g. Most et al 2020;Tews et al 2021;Biswas et al 2021), and comparisons with various maximum NS mass estimates suggest its secondary may be a low-mass BH (Abbott et al 2020b;, we now entertain the scenario in which it is a NS and revisit our population inference under this assumption. Because GW190814 is such an outlier relative to the other GW observations, its inclusion in the population has a significant impact on the inferred mass distribution.…”

Section: Resultsmentioning

confidence: 99%

The Mass Distribution of Neutron Stars in Gravitational-wave Binaries

Landry,

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2021

Preprint

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The discovery of two neutron star-black hole coalescences by LIGO and Virgo brings the total number of likely neutron stars observed in gravitational waves to six. We perform the first inference of the mass distribution of this extragalactic population of neutron stars. In contrast to the bimodal Galactic population detected primarily as radio pulsars, the masses of neutron stars in gravitational-wave binaries are thus far consistent with a uniform distribution, with a greater prevalence of high-mass neutron stars. The maximum mass in the gravitational-wave population agrees with that inferred from the neutron stars in our Galaxy and with expectations from dense matter.

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“…The secondary component is either the lightest black hole or the heaviest NS ever discovered. However, this is still a question of debate [201][202][203][204][205][206][207][208][209].…”

Section: Gravitational Waves 421 Observationmentioning

confidence: 99%

Nuclear Physics and Astrophysics Constraints on the High Density Matter Equation of State

Stone

2021

Universe

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(1) This review has been written in memory of Steven Moszkowski who unexpectedly passed away in December 2020. It has been inspired by our many years of discussions. Steven’s enthusiasm, drive and determination to understand atomic nuclei in simple terms of basic laws of physics was infectious. He sought the fundamental origin of nuclear forces in free space, and their saturation and modification in nuclear medium. His untimely departure left our job unfinished but his legacy lives on. (2) Focusing on the nuclear force acting in nuclear matter of astrophysical interest and its equation of state (EoS), we take several typical snapshots of evolution of the theory of nuclear forces. We start from original ideas in the 1930s moving through to its overwhelming diversity today. The development is supported by modern observational and terrestrial data and their inference in the multimessenger era, as well as by novel mathematical techniques and computer power. (3) We find that, despite the admirable effort both in theory and measurement, we are facing multiple models dependent on a large number of variable correlated parameters which cannot be constrained by data, which are not yet accurate, nor sensitive enough, to identify the theory closest to reality. The role of microphysics in the theories is severely limited or neglected, mostly deemed to be too difficult to tackle. (4) Taking the EoS of high-density matter as an example, we propose to develop models, based, as much as currently possible, on the microphysics of the nuclear force, with a minimal set of parameters, chosen under clear physical guidance. Still somewhat phenomenological, such models could pave the way to realistic predictions, not tracing the measurement, but leading it.

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GW190814: on the properties of the secondary component of the binary

Cited by 60 publications

References 67 publications

Impact of the PSR J0740+6620 radius constraint on the properties of high-density matter

Impact of the PSR J0740+6620 radius constraint on the properties of high-density matter

The Mass Distribution of Neutron Stars in Gravitational-wave Binaries

Nuclear Physics and Astrophysics Constraints on the High Density Matter Equation of State

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