Multimessenger and multiphysics Bayesian inference for the GW170817 binary neutron star merger

Güven, H.; Bozkurt, Kutsal; Khan, E.; Margueron, J.

doi:10.1103/physrevc.102.015805

Cited by 54 publications

(34 citation statements)

References 92 publications

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“…In order to make a legitimate comparison, we show for each hypothesis the posterior distributions before (full lines) and after (histograms) the implementation of the GW170817 filter. Similar to previous analyses employing a large exploration of the nucleonic EOS parameter space [31,82], we can see that our prior distribution only agrees with the high Λ part of the experimental spectrum, that is it suggests considerably high stiffness within the interval compatible with the GW observation ( Λ < 800 at the 90% level, with a low-spin prior and using the PhenomPNRT waveform model in ref. [70]).…”

Section: Ns Static Propertiessupporting

confidence: 83%

A Bayesian analysis of the properties of hybrid stars with the NJL model

Pfaff,

Hansen,

Gulminelli

2021

Preprint

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Section: Ns Static Propertiessupporting

confidence: 83%

A Bayesian analysis of the properties of hybrid stars with the NJL model

Pfaff,

Hansen,

Gulminelli

2021

Preprint

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“…This first detection shows the potential of future GW detections from binary neutron star mergers to constrain the EoS, see e.g. (De et al 2018;Dexheimer et al 2019;Capano et al 2020;Malik et al 2019;Güven et al 2020). There exists in fact a one-to-one relation between a given EoS and the tidal deformability as function of the star's mass (Hinderer et al 2010) similar to the mass-radius diagram (M-R diagram) of cold non-rotating neutron stars.…”

Section: Introductionmentioning

confidence: 63%

What can be learned from a proto-neutron star’s mass and radius?

Preau

Pascal

Novak

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We make extensive numerical studies of masses and radii of proto-neutron stars during the first second after their birth in core-collapse supernova events. We use a quasi-static approach for the computation of proto-neutron star structure, built on parameterized entropy and electron fraction profiles, that are then evolved with neutrino cooling processes. We vary the equation of state of nuclear matter, the proto-neutron star mass and the parameters of the initial profiles, to take into account our ignorance of the supernova progenitor properties. Our results suggest that if masses and radii of a proto-neutron star can be determined in the first second after the birth, e.g. from gravitational wave emission, no information could be obtained on the corresponding cold neutron star and therefore on the cold nuclear equation of state. Similarly, it seems unlikely that any property of the proto-neutron star equation of state (hot and not beta-equilibrated) could be determined either, mostly due to the lack of information on the entropy, or equivalently temperature, distribution in such objects.

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“…More comprehensive Bayesian analyses, including not only gravitational-wave data, but also data from the related electromagnetic emission and other observational and experimental data are also available [23,41,56,93,122,130,155,158,196].…”

Section: Gravitational Waves From the Inspiral Phasementioning

confidence: 99%