Massive relativistic compact stars from SU(3) symmetric quark models

Fu, Han Rui; Li, Jia Jie; Sedrakian, Armen; Weber, Fridolin

doi:10.1016/j.physletb.2022.137470

Cited by 11 publications

(4 citation statements)

References 109 publications

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“…Ref. [75] finds hypernuclear stars with masses close to 2.5M ⊙ can be achieved in the case of maximally fast (Keplerian) rotation, but their values of Q sat are much larger than those considered here. It was concluded that the GW190814 The lower half shows the same quantities for maximally rotating (Keplerian) sequences.…”

Section: Cold Equation Of State and Astrophysical Constraintsmentioning

confidence: 55%

“…The range of inferred masses is within the "mass gap" where neither neutron stars nor black holes were found and are also hard to form with current theoretical models. This scenario has been explored with the DDME2 parametrization with some variations of the hyperonic coupling constants [72][73][74][75]. Ref.…”

Section: Cold Equation Of State and Astrophysical Constraintsmentioning

confidence: 99%

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Finite-temperature equations of state of compact stars with hyperons: three-dimensional tables

Tsiopelas,

Sedrakian,

Oertel

2024

Eur. Phys. J. A

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We construct tables of finite temperature equation of state (EoS) of hypernuclear matter in the range of densities, temperatures, and electron fractions that are needed for numerical simulations of supernovas, proto-neutron stars, and binary neutron star mergers and cast them in the format of CompOSE database. The tables are extracted from a model that is based on covariant density functional (CDF) theory that includes the full $$J^P=1/2^+$$ J P = 1 / 2 + baryon octet in a manner that is consistent with the current astrophysical and nuclear constraints. We employ a parameterization with three different values of the slope of the symmetry energy $$L_\textrm{sym}=30$$ L sym = 30 , 50 and 70 MeV and fixed skewness $$Q_\textrm{sat}= 400$$ Q sat = 400 MeV for above saturation matter. A model for the EoS of inhomogeneous matter is matched at sub-saturation density to the high-density hypernuclear EoS. We discuss the generic features of the resulting EoS and the composition of matter as a function of density, temperature, and electron fraction. The nuclear characteristics and strangeness fraction of these models are compared to the alternatives from the literature. The integral properties of static and rapidly rotating compact stars in the limit of zero temperature are discussed and confronted with the multimessenger astrophysical constraints.

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Section: Cold Equation Of State and Astrophysical Constraintsmentioning

confidence: 55%

Section: Cold Equation Of State and Astrophysical Constraintsmentioning

confidence: 99%

Finite-temperature equations of state of compact stars with hyperons: three-dimensional tables

Tsiopelas,

Sedrakian,

Oertel

2024

Eur. Phys. J. A

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“…Many theoretical attempts have been made to obtain the EOSs of the pure hadron stars, i.e., neutron stars composed of pure nuclear matter and leptons, with different nuclear many-body methods. The density functional theories (DFTs), including the nonrelativistic Skyrme-Hartree-Fock (SHF) [7,8], the relativistic mean field (RMF) [9][10][11] and the relativistic Hartree-Fock (RHF) theory [12,13], are based on effective nucleon-nucleon (NN) interactions, where the parameters are determined by fitting the ground state properties of finite nuclei and the empirical saturation properties of infinite nuclear matter. However, the effective NN interactions are loosely constrained at higher densities, and the predictions of the neutron star properties with different DFTs are rather divergent.…”

Section: Introductionmentioning

confidence: 99%

Hadron-quark phase transition in neutron star by combining the relativistic Brueckner-Hartree-Fock theory and Dyson-Schwinger equation approach

Pianpian¹,

Bai²,

Wang³

et al. 2023

Preprint

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Starting from the relativistic Brueckner-Hartree-Fock theory for nuclear matter and the Dyson-Schwinger equation approach for quark matter, the possible hadron-quark phase transition in the interior of neutron star is explored. The first-order phase transition and crossover are studied by performing the Maxwell construction and 3-window construction respectively. The mass-radius relation and the tidal deformability of the hybrid star are calculated and compared to the joint mass-radius observation of neutron star and the constraints from gravitational wave detection. For the Maxwell construction, no stable quark core is found in the interior of a neutron star. For the 3-window construction, the parameters of the smooth interpolation function are chosen in such a way to keep the thermodynamic stability and lead to a moderate crossover density region. To support a two-solar-mass neutron star under the 3-window construction, the effective width of medium screening effects in quark matter should be around 0.35 GeV.

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“…Within the relativistic mean field theory, various attempts to solve the hyperon puzzle are known, e.g., refs. [22][23][24][25][26][27][28][29][30][31][32]. Essentially, a sufficient repulsion at short baryon-baryon distances due to usual and/or hidden strangeness vector fields is introduced to resolve the puzzle.…”

Section: Introductionmentioning

confidence: 99%

Hyperonic Interactions in Neutron Stars

Mikheev,

Lanskoy,

Nasakin

et al. 2023

Particles

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The matter of neutron stars is characterised by the density of the order of typical nuclear densities; hence, it can be described with methods of nuclear physics. However, at high densities, some effects that are absent in nuclear and hypernuclear physics can appear, and this makes neutron stars a good place for studying the properties of baryonic interactions. In the present work, we consider neutron stars consisting of nucleons, leptons and Λ hyperons with Skyrme baryonic forces. We study the character of the ΛN interactions taking place in neutron stars at high densities. In particular, we show the difference between three-body ΛNN and density-dependent ΛN forces. We also demonstrate that the Skyrme ΛN forces proportional to nuclear density are better suited for the modelling of neutron stars than the forces proportional to fractional powers of density. Finally, we emphasize the importance of the point of appearance of hyperons in a further search for parameterizations which are suitable for describing neutron stars.

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Massive relativistic compact stars from SU(3) symmetric quark models

Cited by 11 publications

References 109 publications

Finite-temperature equations of state of compact stars with hyperons: three-dimensional tables

Finite-temperature equations of state of compact stars with hyperons: three-dimensional tables

Hadron-quark phase transition in neutron star by combining the relativistic Brueckner-Hartree-Fock theory and Dyson-Schwinger equation approach

Hyperonic Interactions in Neutron Stars

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