Equation of state in hybrid stars and the stability window of quark matter

Wen, Xin-Jian

doi:10.1016/j.physa.2013.05.050

Cited by 14 publications

(7 citation statements)

References 62 publications

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“…Hence, there may be a possibility that the pulsars which are detected as neutron stars (NSs) may also be quark stars (QSs). SQM, if exist, may play a crucial role in the various remarkable fields such as hot and dense matter in heavy-ion collisions [4][5][6], compact stars structure [7], deconfinement phase transition [8][9][10][11][12][13] etc. The possibility for the existence or non-existence of various phases of compact stars is strongly constrained by the astrophysical data on pulsars.…”

Section: Introductionmentioning

confidence: 99%

Properties of strange quark matter and strange quark stars

Kumari

Kumar

2021

Eur. Phys. J. C

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A Polyakov chiral $$\text {SU(3)}$$ SU(3) quark mean-field (PCQMF) model is applied to study the properties of strange quark matter (SQM) and strange quark star (SQS) in $$\beta $$ β -equilibrium. The effect of increasing the strength of vector interactions on the effective constituent quark mass, particle fractions, and the thermodynamical properties such as pressure, energy density, and the speed of sound is investigated. We investigate the above properties for the SQM relevant for various stages of star evolution, i.e., considering with/without trapped neutrinos and zero/finite entropy. The finite lepton fraction and the entropy of the medium is observed to cause the stiffness in the equation of state (EoS). Finally, we calculate the mass-radius relation and the dimensionless tidal deformability within the present model calculations and compare the results to the recent studies.

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Section: Introductionmentioning

confidence: 99%

Properties of strange quark matter and strange quark stars

Kumari

Kumar

2021

Eur. Phys. J. C

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“…Since its possible absolute stability was conjectured nearly thirty years ago [1], strange quark matter (SQM) has been playing an important role in many interesting fields, for example, the deconfinement phase transition [2][3][4][5][6][7], the hot and dense matter in heavy ion collisions [8], the structure of compact stars [9], etc. Lumps of SQM, the so-called strangelets [10], or slets [11], may exist in cosmic rays [12], and some of them might be on the way to our Earth [13,14].…”

Section: Introductionmentioning

confidence: 99%

Thermodynamic consistency, quark mass scaling, and properties of strange matter

et al. 2014

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The previous thermodynamic treatment for models with density and/or temperature dependent quark masses is shown to be inconsistent with the requirement of fundamental thermodynamics. We therefore study a fully self-consistent one according to the fundamental differential equation of thermodynamics. After obtaining a new quark mass scaling with the inclusion of both confinement and leading-order perturbative interactions, we investigate properties of strange quark matter in the fully consistent thermodynamic treatment. It is found that the equation of state become stiffer, and accordingly, the maximum mass of strange stars is as large as about 2 times the solar mass, if strange quark matter is absolutely or metastable.

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“…The droplets made of SQM, namely strangelets or slets [4][5][6][7], could serve as a unique signature for the formation of quark gluon plasma (QGP) in the experiments of relativistic heavy-ion collision. A through investigation on the properties of SQM is thus crucial for us to understand various astrophysical phenomena as well as the QCD phase transition mechanisms [8][9][10][11][12].…”

Section: Introductionmentioning

confidence: 99%

Strange quark matter and proto-strange stars in an equivaparticle model

Chen¹,

Xia²,

Peng³

2021

Preprint

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The properties of strange quark matter and the structures of (proto-)strange stars are studied within the framework of an equivparticle model, where a new quark mass scaling and self-consistent thermodynamic treatment are adopted. Our results show that the perturbative interaction has a strong impact on the properties of strange quark matter. It is found that the energy per baryon increases with temperature, while the free energy decreases and eventually becomes negative. At fixed temperatures, the pressure at the minimum free energy per baryon is zero, suggesting that the thermodynamic self-consistency is preserved. Additionally, the sound velocity v in quark matter approaches to the extreme relativistic limit (c/ √ 3) as the density increases. By increasing the strengths of confinement parameter D and perturbation parameter C, the tendency for v to approach the extreme relativistic limit at high density is slightly weakened. For (proto-)strange stars, in contrast to the quark mass scalings adopted in previous publications, the new quark mass scaling can accommodate massive proto-strange stars with their maximum mass surpassing twice the solar mass at T = 50 MeV.

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Equation of state in hybrid stars and the stability window of quark matter

Cited by 14 publications

References 62 publications

Properties of strange quark matter and strange quark stars

Properties of strange quark matter and strange quark stars

Thermodynamic consistency, quark mass scaling, and properties of strange matter

Strange quark matter and proto-strange stars in an equivaparticle model

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