Structure of the hadron-quark mixed phase in protoneutron stars

Chen, H.; Burgio, G. F.; Schulze, H.-J.; Yasutake, Nobutoshi

doi:10.1051/0004-6361/201220718

Cited by 31 publications

(25 citation statements)

References 73 publications

(103 reference statements)

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“…As in the case of the pseudo-quark forming, initially is formed a pre-cluster M z * of pseudo-quarks q 0 , which is confined in a super-strong magnetic field, ξ B -which may explains also the cold genesis of electrons, by dark photons confining around a superdense centroid, resulted by quantons confining in the field of chiral fluctuations of primordial dark energy, according to CGT, [4]. Extrapolating the previous conclusions for the case of cold quarks cluster forming, it results logically the possibility of quasi-cristallin quarks networks forming, considered also for the stelary structures forming, (quark star, [11], [12]), but also the possibility of multi-quark particles forming, (tetra-, penta-, hexa-, hepta-quark particles), possibility which was sustained theoretically and was experimentally confirmed, [13].…”

Section: The Mechanism Of Preonic Cold Quarks Forming and Of Dark Matmentioning

confidence: 93%

The Explaining of the Elementary Particles Cold Genesis by a Preonic Quasi-Crystal Model of Quarks and a Pre-Quantum Theory of Fields

Arghirescu¹

2018

IJHEP

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Through a preonic quasi-crystalline quark model, resulted as Bose-Einstein condensate of gammons: γ * = (e + e-) and by a pre-quantum cold genesis theory of matter and fields, which predicted the existence of a preon z 0 ≈ 34 m e experimentally evidenced in 2015, the elementary particles genesis is explained by the cold genesis of two preonic bosons with hexagonal symmetry: z π = 7z 0 ; z 2 = 4z 0 , which explains also the stability of quarks, by a mechanism with a first step of z * /(q ± /q 0) *-pre-cluster forming by magnetic interaction and a second step of z/(q ± /q 0)-collapsed cluster forming , with the aid of magnetic confinement, with z = (z 0 , z 2 , z π) and (q ± /q 0)-quark or pseudo-quark, resulting some predictions for bosonic dark matter constituents and for multi-quark particles of cold genesis, such as: 2450 m e ; 2685.4 m e tetra-quark; 3063.8 m e pentaquark; 2720 m e , 3672.4 m e hexa-quark; 3329 m e , 4762.2 m e hepta-quark.

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Section: The Mechanism Of Preonic Cold Quarks Forming and Of Dark Matmentioning

confidence: 93%

The Explaining of the Elementary Particles Cold Genesis by a Preonic Quasi-Crystal Model of Quarks and a Pre-Quantum Theory of Fields

Arghirescu¹

2018

IJHEP

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“…These are the well-known chemical equilibrium conditions that are generally used to determine the composition of the hot matter under β equilibrium (Nicotra et al 2006;Peng et al 2008;Li et al 2010;Burgio et al 2011;Chen et al 2013). …”

Section: β Equilibrium Of the Hot Nuclear Mattermentioning

confidence: 99%

“…Incorporating the strong interaction between nucleons will certainly affect the constituent chemical potentials, the composition, and the EoS of the matter. The employed nuclear model is the microscopic Brueckner-Hartree-Fock (BHF) approach widely used for studying dense stellar matter and neutron star properties (Baldo et al 1997;Baldo 1999;Baldo & Ferreira 1999;Burgio et al 2003;Zuo et al 2004;Li et al 2006Li et al , 2010Nicotra et al 2006;Peng et al 2008;Burgio et al 2011;Chen et al 2013), as we discuss in Sect. 2.2.…”

Section: Introductionmentioning

confidence: 99%

Revisiting the hot matter in the center of gamma-ray bursts and supernovae

Liu

2013

A&A

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Aims. Hot matter with nucleons can be produced in the inner region of the neutrino-dominated accretion flow in gamma-ray bursts or during the proto-neutron star birth in successful supernovae. The composition and equation of state of the matter depend on the dynamic β equilibrium under various neutrino opacities. The strong interaction between nucleons may also play an important role. We plan to extend the previous studies by incorporating these two aspects in our model. Methods. The modification of the β-equilibrium condition from neutrino optically thin to thick was modeled by an equilibrium factor χ ranging between the neutrino-freely-escaping case and the neutrino-trapped case. We employed the microscopic BruecknerHartree-Fock approach extended to the finite temperature regime to study the interacting nucleons. Results. We show the composition and chemical potentials of the hot nuclear matter for different densities and temperatures at each stage of β equilibrium. We also compare our realistic equation of states with those of the free-gas model. We find that it is important to properly describe the neutrino opacity and the strong interaction between nucleons, and they should be taken into account in model calculations.

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“…In several recent papers [18][19][20][21][22][23][24], it has been shown that they may contain significant fractions of quark-hybrid matter in their centers, despite the relatively stiff nuclear equation of state (EoS) that is required to achieve such high masses. The radii of these neutron stars would be between 13 and 14 km, depending on the nuclear EoS [18,19], increasing to respectively 13.5 and 14.5 km for lighter neutron stars with canonical masses of around 1.4 M ⊙ .…”

Section: Introductionmentioning

confidence: 99%

Thermal evolution of hybrid stars within the framework of a nonlocal Nambu–Jona-Lasinio model

et al. 2015

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We study the thermal evolution of neutron stars containing deconfined quark matter in their core. Such objects are generally referred to as quark-hybrid stars. The confined hadronic matter in their core is described in the framework of non-linear relativistic nuclear field theory. For the quark phase we use a non-local extension of the SU(3) Nambu Jona-Lasinio model with vector interactions. The Gibbs condition is used to model phase equilibrium between confined hadronic matter and deconfined quark matter. Our study indicates that high-mass neutron stars may contain between 35 and 40% deconfined quark-hybrid matter in their cores. Neutron stars with canonical masses of around 1.4 M⊙ would not contain deconfined quark matter. The central proton fractions of the stars are found to be high, enabling them to cool rapidly. Very good agreement with the temperature evolution established for the neutron star in Cassiopeia A (Cas A) is obtained for one of our models (based on the popular NL3 nuclear parametrization), if the protons in the core of our stellar models are strongly paired, the repulsion among the quarks is mildly repulsive, and the mass of Cas A has a canonical value of 1.4 M⊙.

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Structure of the hadron-quark mixed phase in protoneutron stars

Cited by 31 publications

References 73 publications

The Explaining of the Elementary Particles Cold Genesis by a Preonic Quasi-Crystal Model of Quarks and a Pre-Quantum Theory of Fields

The Explaining of the Elementary Particles Cold Genesis by a Preonic Quasi-Crystal Model of Quarks and a Pre-Quantum Theory of Fields

Revisiting the hot matter in the center of gamma-ray bursts and supernovae

Thermal evolution of hybrid stars within the framework of a nonlocal Nambu–Jona-Lasinio model

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