Bayesian reconstruction of nuclear matter parameters from the equation of state of neutron star matter

Imam, S.; Patra, N. K.; Mondal, C.; Malik, Tuhin; Agrawal, B. K.

doi:10.1103/physrevc.105.015806

Cited by 27 publications

(19 citation statements)

References 76 publications

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“…The objective of the present study is to confront the phenomenological hyperonic interaction to the recently observed neutron star properties (like mass M , radius R and tidal deformability Λ), and perform Bayesian inference for the hyperon-meson coupling constants from the robust LIGO/Virgo tidal measurement of the GW170817 binary neutron star merger (Abbott et al 2017) 1 as well as two NICER mass-radius measurements of pulsars [PSR J0030+0451 (Riley et al 2019;Miller et al 2019) and PSR J0740+6620 (Riley et al 2021;Miller et al 2021)]. Previously, such kind of Bayesian analysis on nuclear matter parameters has been performed in, e.g., Traversi & Char (2020); Imam et al (2022); Malik et al (2022), we here focus on the hypernuclear matter based on a set of six generally-used relativistic mean-field (RMF) Lagrangians. We consider two different classes of the RMF models, one with constant couplings and nonlinear meson terms in the Lagrangian [NL3ωρ (Horowitz & Piekarewicz 2001), PK1 (Long et al 2004)] and a second one without these terms but introducing density-dependent coupling strengths [DD-LZ1 (Wei et al 2020), DD-ME2 (Lalazissis et al 2005), DD2 (Typel et al 2010), PKDD (Long et al 2004)], which all treat effectively the in-medium properties of baryon-baryon interaction.…”

Section: Introductionmentioning

confidence: 99%

Astrophysical implications on hyperon couplings and hyperon star properties with relativistic equations of states

Sun¹,

Miao²,

Sun³

et al. 2022

Preprint

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Hyperons are essential constituents in the neutron star interior. The poorly-known hyperonic interaction is a source of uncertainty for studying laboratory hypernuclei and neutron star observations. In this work, we perform Bayesian inference of phenomenological hyperon-nucleon interactions using the tidal-deformability measurement of the GW170817 binary neutron star merger as detected by LIGO/Virgo and the mass-radius measurements of PSR J0030+0541 and PSR J0740+6620 as detected by NICER. The analysis is based on six relativistic neutron-star-matter equation of states with hyperons from the relativistic mean-field theory, naturally fulfilling the causality requirement and empirical nuclear matter properties. We specifically utilize the strong correlation recently deduced between the scalar and vector meson hyperon couplings, imposed by the measured Λ separation energy in single-Λ hypernuclei, and perform four different tests with or without the strong correlation. We find that the laboratory hypernuclear constraint ensures a large enough Λ-scalar-meson coupling to match the large vector coupling in hyperon star matter. When adopting the current most probable intervals of hyperon couplings from the joint analysis of laboratory and astrophysical data, we find the maximum mass of hyperon stars is at most 2.176 +0.085 −0.202 M (1σ credible interval) from the chosen set of stiff equation of states. The reduction of the stellar radius due to hyperons is quantified based on our analysis and various hyperon star properties are provided.

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Section: Introductionmentioning

confidence: 99%

Astrophysical implications on hyperon couplings and hyperon star properties with relativistic equations of states

Sun¹,

Miao²,

Sun³

et al. 2022

Preprint

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“…Still another problem is the determination of the star composition once the EOS is known. Some recent studies have shown that the extraction of the neutron star composition is not trivial even if the problem is restricted to the proton fraction de Tovar et al ( 2021); Imam et al (2022); Mondal & Gulminelli (2021); Essick et al (2021b). The present study will add another contribution to this topic, but now considering also non-nucleonic degrees of freedom.…”

Section: Introductionmentioning

confidence: 77%

“…with ρ p , ρ Ξ − , ρ e and ρ µ the number density of protons, cascades, electrons and muons, respectively. For the crust EOS, the procedure described in Malik et al (2022) will be considered: the outer crust is described by the Bethe-Pethick-Sutherland (BPS) EOS; The outer crust and the core are joined using a polytropic function Carriere et al (2003) p(ε) = a 1 + a 2 ε γ , where the parameters a 1 and a 2 are determined in such a way that the EOS for the inner crust joins the upper layer of the outer crust at (ρ = 10 −4 fm −3 ) to the core EOS at (ρ = 0.04 fm −3 ). The polytropic index γ is taken to be equal to 4/3.…”

Section: Modelmentioning

confidence: 99%

“…In the following, we will consider large sets of models that satisfy not only the two solar mass NS constraints but also the PNM constraints from Hebeler et al (2013) and reanalyze the conclusions drawn in Fortin et al (2015). Starting from a relativistic mean field description of stellar matter, considering a field theoretical model with density dependent couplings to the meson fields (DDH) as introduced in Malik et al (2022), we will include hyperonic degrees of freedom and will determine the occurrence probability of different nuclear matter properties (NMPs) and stellar properties, within a Bayesian inference framework. Notice that we are assisting to a wider and wider interest on the problem of extracting the EOS of stellar matter from the knowledge of observational data, generally using statistical methods such as Bayesian inference Ozel et al (2010); Steiner et al (2010Steiner et al ( , 2013; Ozel et al (2016); Raithel et al (2016Raithel et al ( , 2017 or non-parametric inference Landry & Essick (2019); Essick et al (2020); Landry et al (2020) or deep machine learning techniques Fujimoto et al (2018Fujimoto et al ( , 2020; ; Morawski & Bejger (2020).…”

Section: Introductionmentioning

confidence: 99%

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Bayesian inference of signatures of hyperons inside neutron stars

Malik¹,

Providência²

2022

Preprint

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Context. Recent developments in multi-messenger astronomy bring important information on matter far beyond the one reachable in terrestrial laboratories, as matter existing inside neutron stars (NS). As a consequence, there is a large interest on the problem of extracting the equation of state of stellar matter as well as of determining the internal composition of NS from the knowledge of observational data generally using statistical methods. Aims. Determine possible signatures of the presence of hyperons inside neutron stars, using a set of EOS that satisfy laboratory, theoretical and observational constraints. Methods. Three sets of models of 15000 equations of state (EOS) based on a density dependent relativistic mean field description of hadronic matter are built. One of the sets is restricted to nucleonic matter, the second set includes Λ-hyperons and nucleons and the third set includes Λ and Ξ − -hyperons and nucleons. Electrical neutrality and β-equilibrium are imposed in the three sets. Nuclear matter properties, hypernuclei properties and observational information are used to constraint the models within a Bayesian inference approach.Results. General properties of neutron stars such as the maximum mass, radius, tidal deformability, proton fraction, hyperon fraction and speed of sound are discussed. It is shown that the two solar mass constraint imposes that neutron stars described by equations of state that include hyperons have in average a larger radius, 0.5km, and a larger tidal deformability, 150, than the stars determined from a nucleonic equation of state, while the speed of sound at the center of the star is more than 25% smaller. Conclusions. If a 1.4 M star with a radius 12.5 km is measured it is quite improbable that a massive star described by the same model contains hyperons. A similar conclusion is drawn if a two solar mass star with a radius 11.5 km or a neutron star with a mass above 2.2 M is observed: the possible hyperon content of these stars is ruled out or very reduced. The hyperon presence inside neutron stars is compatible with the present NICER mass-radius observations of the pulsars PSR J0030+0451 and PSR J0740+6620 and the gravitational wave detection GW170817.

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“…Another approach has been considered that also spans an acceptable NS mass-radius domain such as a Taylor expansion parameterization of the EOS (Margueron et al 2018a(Margueron et al , 2018bZhang et al 2018;Ferreira & Providência 2021b;Ferreira & Providência 2021a). The recovery of the nuclear matter properties from the β-equilibrium EOS has proven to be impossible without the knowledge of the compositions or symmetry energy at high densities (de Tovar et al 2021;Imam et al 2022; or the knowledge of the EOS of symmetric nuclear matter along with compositions (Essick et al 2021b).…”

Section: = -+mentioning

confidence: 99%

Relativistic Description of Dense Matter Equation of State and Compatibility with Neutron Star Observables: A Bayesian Approach

Malik

Ferreira

Agrawal

et al. 2022

ApJ

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The general behavior of the nuclear equation of state (EOS), relevant for the description of neutron stars (NSs), is studied within a Bayesian approach applied to a set of models based on a density-dependent relativistic mean-field description of nuclear matter. The EOS is subjected to a minimal number of constraints based on nuclear saturation properties and the low-density pure neutron matter EOS obtained from a precise next-to-next-to-next-to-leading order (N3LO) calculation in chiral effective field theory (χEFT). The posterior distributions of the model parameters obtained under these minimal constraints are employed to construct the distributions of various nuclear matter properties and NS properties such as radii, tidal deformabilities, central energy densities, speeds of sound, etc. We found that a 90% confidence interval for the allowed NS mass–radius relationship and tidal deformabilities is compatible with GW170817 and recent Neutron star Interior Composition ExploreR observations, without invoking the exotic degrees of freedom. A central speed of sound of the order of 2 / 3 c is obtained. The maximum NS mass allowed by the model is 2.5 M ⊙.

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Bayesian reconstruction of nuclear matter parameters from the equation of state of neutron star matter

Cited by 27 publications

References 76 publications

Astrophysical implications on hyperon couplings and hyperon star properties with relativistic equations of states

Astrophysical implications on hyperon couplings and hyperon star properties with relativistic equations of states

Bayesian inference of signatures of hyperons inside neutron stars

Relativistic Description of Dense Matter Equation of State and Compatibility with Neutron Star Observables: A Bayesian Approach

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