Effect of color superconductivity on the mass and radius of a quark star

Rüster, Stefan B.; Rischke, Dirk H.

doi:10.1103/physrevd.69.045011

Cited by 95 publications

(88 citation statements)

References 33 publications

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“…The hadron-quark phase transition is one of the most concerned topics, and so far it is still controversial whether quarks can appear in cold neutron star [34][35][36][37][38]. It is also an important topic in heavy-ion collisions, and related experiments at medium and high densities will be performed in the near future on the updated facilities of NICA at JINR-Dubna and FAIR at GSI-Darmstadt.…”

Section: Introductionmentioning

confidence: 99%

Isoscalar-vector interaction and hybrid quark core in massive neutron stars

et al. 2013

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The hadron-quark phase transition in the core of massive neutron stars is studied with a newly constructed two-phase model. For nuclear matter, a nonlinear Walecka type model with general nucleon-meson and meson-meson couplings, recently calibrated by Steiner, Hemper and Fischer, is taken. For quark matter, a modified Polyakov-Nambu-Jona-Lasinio (mPNJL) model, which gives consistent results with lattice QCD data, is used. Most importantly, we introduce an isoscalar-vector interaction in the description of quark matter, and we study its influence on the hadron-quark phase transition in the interior of massive neutron stars. With the constraints of neutron star observations, our calculation shows that the isoscalar-vector interaction between quarks is indispensable if massive hybrids star exist in the universe, and its strength determines the onset density of quark matter, as well as the mass-radius relations of hybrid stars. Furthermore, as a connection with heavy-ioncollision experiments we give some discussions about the strength of isoscalar-vector interaction and its effect on the signals of hadron-quark phase transition in heavy-ion collisions, in the energy range of the NICA at JINR-Dubna and FAIR at GSI-Darmstadt facilities.

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Section: Introductionmentioning

confidence: 99%

Isoscalar-vector interaction and hybrid quark core in massive neutron stars

et al. 2013

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“…Studies prior to the discovery pulsar PSR J1614-2230 have suggested the stiffening quark matter EOS from the effect of strong interactions, such as one-gluon exchange or colorsuperconductivity [11][12][13][14][15][16][17], which can satisfy the new constraint. Ozel [18] and Lattimer [19] gave first studies on the implications of the new mass limits from PSR J1614-2230 for quark and hybrid stars in the quark bag model.…”

Section: Introductionmentioning

confidence: 99%

Maximum mass of a hybrid star having a mixed-phase region based on constraints set by the pulsar PSR J1614-2230

Mallick

2013

Phys. Rev. C

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Recent observation of pulsar PSR J1614-2230 with mass about 2 solar masses poses a severe constraint on the equations of state (EOS) of matter describing stars under extreme conditions. Neutron stars (NS) can reach the mass limits set by PSR J1614-2230. But stars having hyperons or quark stars (QS) having boson condensates, with softer EOS can barely reach such limits and are ruled out. QS with pure strange matter also cannot have such high mass unless the effect of strong coupling constant or color superconductivity are considered. In this work I try to calculate the upper mass limit for a hybrid stars (HS) having a quark-hadron mixed phase. The hadronic matter (having hyperons) EOS is described by relativistic mean field theory and for the quark phase I use the simple MIT bag model. I construct the intermediate mixed phase using Glendenning construction. HS with a mixed phase cannot reach the mass limit set by PSR J1614-2230 unless I assume a density dependent bag constant. For such case the mixed phase region is small. The maximum mass of a mixed hybrid star obtained with such mixed phase region is 2.01M ⊙ .

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“…to its mass/radius relation, one would have an observational tool to discriminate among the actual realization of different star inner phases in nature. From previous theoretical studies [4,8,10,11,18,23,40,101,102,117,118,126,129] the mass-radius relationship predicted for neutron stars with different quark-matter phases (CS or unpaired) at the core are very similar to those having hadronic phases, at least for the observed mass/radius range. As a consequence, it is very difficult to find a clear observational signature that can distinguish among them.…”

Section: Equation Of State Of the Mcfl Phasementioning

confidence: 99%

Magnetism in Dense Quark Matter

Ferrer

Incera

2013

Strongly Interacting Matter in Magnetic Fields

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We review the mechanisms via which an external magnetic field can affect the ground state of cold and dense quark matter. In the absence of a magnetic field, at asymptotically high densities, cold quark matter is in the Color-Flavor-Locked (CFL) phase of color superconductivity characterized by three scales: the superconducting gap, the gluon Meissner mass, and the baryonic chemical potential. When an applied magnetic field becomes comparable with each of these scales, new phases and/or condensates may emerge. They include the magnetic CFL (MCFL) phase that becomes relevant for fields of the order of the gap scale; the paramagnetic CFL, important when the field is of the order of the Meissner mass, and a spin-one condensate associated to the magnetic moment of the Cooper pairs, significant at fields of the order of the chemical potential. We discuss the equation of state (EoS) of MCFL matter for a large range of field values and consider possible applications of the magnetic effects on dense quark matter to the astrophysics of compact stars.

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Effect of color superconductivity on the mass and radius of a quark star

Cited by 95 publications

References 33 publications

Isoscalar-vector interaction and hybrid quark core in massive neutron stars

Isoscalar-vector interaction and hybrid quark core in massive neutron stars

Maximum mass of a hybrid star having a mixed-phase region based on constraints set by the pulsar PSR J1614-2230

Magnetism in Dense Quark Matter

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