scholarly journals Quark star matter at finite temperature in a quasiparticle model

2021 ◽  
Vol 81 (7) ◽  
Author(s):  
Peng-Cheng Chu ◽  
Yao-Yao Jiang ◽  
He Liu ◽  
Zhen Zhang ◽  
Xiao-Min Zhang ◽  
...  
Keyword(s):  
Quark Matter ◽  
Strange Quark ◽  
Large Mass ◽  
Compact Stars ◽  
Heating Process ◽  
Maximum Mass ◽  
Quark Stars ◽  
Star Evolution ◽  
Quasiparticle Model ◽  
Effects Of Temperature

AbstractWe study the thermodynamic properties of asymmetric quark matter, large mass quark stars (QSs), and proto-quark stars (PQSs) within the quasiparticle model. Considering the effects of temperature within quasiparticle model can significantly influence the EOS and the entropy of strange quark matter (SQM), quark fractions in SQM, as well as the tidal deformability and the maximum mass of PQSs along the star evolution line. Our results indicate that the recent discovered heavy compact stars PSR J0348+0432, MSR J0740+6620, PSR J2215+5135, and especially the GW190814’s secondary component $$m_2$$ m 2 can be well described as QSs within the quasiparticle model. The tidal deformability for the QSs describing the heavy compact stars is extremely large, which can not well describe GW170817 as QSs, and the effects of the temperature in the heating process along the star evolution will further increase the tidal deformability and the maximum mass of PQSs.

scholarly journals Properties of strange quark matter and strange quark stars

2021 ◽  
Vol 81 (9) ◽  
Author(s):  
Manisha Kumari ◽  
Arvind Kumar
Keyword(s):  
Quark Matter ◽  
Strange Quark ◽  
Present Model ◽  
Constituent Quark ◽  
Mean Field ◽  
Strange Quark Matter ◽  
Model Calculations ◽  
Quark Stars ◽  
Star Evolution ◽  
Constituent Quark Mass

AbstractA 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.

scholarly journals Quark star matter in heavy quark stars

2021 ◽  
Vol 81 (1) ◽  
Author(s):  
Peng-Cheng Chu ◽  
Yi Zhou ◽  
Yao-Yao Jiang ◽  
Hong-Yang Ma ◽  
He Liu ◽  
...  
Keyword(s):  
Thermodynamic Properties ◽  
Quark Matter ◽  
Quark Mass ◽  
Orientation Distribution ◽  
Large Mass ◽  
Compact Stars ◽  
Credibility Interval ◽  
Quark Star ◽  
Mass Model ◽  
Quark Stars

AbstractWe study the thermodynamic properties of asymmetric quark matter and large mass quark stars within the confined-isospin-density-dependent-quark-mass model. We find that the quark matter symmetry energy should be very large in order to describe the recent discovered heavy compact stars PSR J0348+0432 ($$\text {2.01}\pm \text {0.04}M_{\odot }$$ 2.01 ± 0.04 M ⊙ ), MSP J0740+6620 ($$\text {2.14}\pm ^\text {0.10}_\text {0.09}M_{\odot }$$ 2.14 ± 0.09 0.10 M ⊙ of 68.3$$\%$$ % credibility interval and $$\text {2.14}\pm ^\text {0.20}_\text {0.18}M_{\odot }$$ 2.14 ± 0.18 0.20 M ⊙ of 95.4$$\%$$ % credibility interval) and PSR J2215+5135 (2.27$$\pm ^\text {0.10}_\text {0.09}M_{\odot }$$ ± 0.09 0.10 M ⊙ ) as QSs. The tidal deformability $$\Lambda _{1.4}$$ Λ 1.4 of the QSs is also investigated in this work, and the result indicates that $$\Lambda _{1.4}$$ Λ 1.4 may depend on the isospin effects and the strength / orientation distribution of the magnetic fields inside the quark stars.

Strange quark mass effect on the structure of hybrid stars

2018 ◽  
Vol 27 (01) ◽  
pp. 1850006 ◽  
Author(s):  
Jian-Feng Xu ◽  
Yan-An Luo ◽  
Lei Li ◽  
Guang-Xiong Peng
Keyword(s):  
Quark Matter ◽  
Quark Mass ◽  
Strange Quark ◽  
Mass Effect ◽  
Compact Stars ◽  
Model Parameters ◽  
Maximum Mass ◽  
Strange Quark Mass ◽  
Wide Range ◽  
Hybrid Stars

We study the strange quark mass effect on the phase diagram of strong interaction and the structure of compact stars with a thermodynamically enhanced perturbative QCD model by matching quark matter onto nuclear matter using the Gibbs conditions. It is found that the mass effect of strange quark matter can obviously stiffen the equation of state of mixed phases and result in more massive hybrid stars (HSs), while that usually lowers the maximum mass of pure quark stars. Given reasonable model parameters, the maximum mass of HSs can reach two times the solar mass and the stars always have mixed-phase core in a considerably wide range of model parameters.

A 2M⊙ PULSAR: IMPLICATIONS FOR QUARK MATTER

2011 ◽  
Vol 20 (supp02) ◽  
pp. 117-124
Author(s):  
XIAOYU LAI ◽  
RENXIN XU
Keyword(s):  
Quark Matter ◽  
Dense Matter ◽  
State Equation ◽  
The State ◽  
Point Of View ◽  
Compact Stars ◽  
Maximum Mass ◽  
Quantum Chromo Dynamics ◽  
Quark Stars ◽  
High Maximum

The state of cold quark matter at supra-nuclear density, depending on the non-perturbative nature of quantum chromo-dynamics (QCD), is essential for modelling pulsars. It is conventionally thought that the state equation of dense matter softens and thus cannot result in high maximum mass if pulsars are quark stars. However, this standard point of view would be revisited and updated if the strong coupling between quarks at realistic baryon densities of compact stars could render quarks grouped in quark-clusters, because the state equation of clustering quark matter stiffs to support compact stars with maximum mass M max > 2M⊙. Although the hypothetical quark-clusters has not been confirmed due to the lack of both theoretical and experimental evidence, the astrophysical observations of pulsars (e.g. pulsar-mass) could help us to explore the properties of cold quark matter.

Strange Quark Matter as Dark Matter

2019 ◽  
Vol 22 (4) ◽  
pp. 311-317
Author(s):  
Hidezumi Terazawa
Keyword(s):  
Dark Matter ◽  
Quark Matter ◽  
Strange Quark ◽  
Strange Quark Matter ◽  
Quark Stars

New forms of matter such as super-hypernuclei (strange quark matter) and superhypernuclear stars (strange quark stars) as candidates for dark matter are discussed in some detail, based on the so-called "Bodmer–Terazawa–Witten hypothesis" assuming that they are stable absolutely or quasi-stable (decaying only weakly).

Quark matter in the perturbation QCD model with a rapidly convergent matching-invariant running coupling

2017 ◽  
Vol 26 (06) ◽  
pp. 1750034 ◽  
Author(s):  
Jian-Feng Xu ◽  
Yan-An Luo ◽  
Lei Li ◽  
Guang-Xiong Peng
Keyword(s):  
Perturbation Theory ◽  
Infinite Number ◽  
Quark Matter ◽  
Chemical Potential ◽  
Maximum Mass ◽  
Solar Mass ◽  
Quark Stars ◽  
Dense Quark Matter ◽  
Subtraction Point ◽  
Running Coupling

The properties of dense quark matter are investigated in the perturbation theory with a rapidly convergent matching-invariant running coupling. The fast convergence is mainly due to the resummation of an infinite number of known logarithmic terms in a compact form. The only parameter in this model, the ratio of the renormalization subtraction point to the chemical potential, is restricted to be about 2.64 according to the Witten–Bodmer conjecture, which gives the maximum mass and the biggest radius of quark stars to be, respectively, two times the solar mass and 11.7[Formula: see text]km.

Quark matter and quark stars within the quasiparticle model under magnetic fields

2021 ◽  
Vol 104 (4) ◽  
Author(s):  
Peng-Cheng Chu ◽  
Xiao-Hua Li ◽  
He Liu ◽  
Jia-Wei Zhang
Keyword(s):  
Magnetic Fields ◽  
Quark Matter ◽  
Quark Stars ◽  
Quasiparticle Model

scholarly journals Maximum Mass of Differentially Rotating Strange Quark Stars

2019 ◽  
Vol 879 (1) ◽  
pp. 44 ◽  
Author(s):  
Magdalena Szkudlarek ◽  
Dorota Gondek-Rosińska ◽  
Loïc Villain ◽  
Marcus Ansorg
Keyword(s):  
Strange Quark ◽  
Maximum Mass ◽  
Quark Stars

scholarly journals QUARK STARS ADMITTING A ONE-PARAMETER GROUP OF CONFORMAL MOTIONS

2004 ◽  
Vol 13 (01) ◽  
pp. 149-156 ◽  
Author(s):  
M. K. MAK ◽  
T. HARKO
Keyword(s):  
Analytical Solution ◽  
Quark Matter ◽  
Spherical Symmetry ◽  
Total Mass ◽  
Strange Quark ◽  
Exact Analytical Solution ◽  
Quark Star ◽  
Parameter Group ◽  
Quark Stars

An exact analytical solution describing the interior of a charged strange quark star is found under the assumption of spherical symmetry and the existence of a one-parameter group of conformal motions. The solution describes a unique static charged configuration of quark matter with radius R=9.46 km and total mass M=2.86M⊙.

scholarly journals Strange matter in compact stars

2018 ◽  
Vol 171 ◽  
pp. 08001 ◽  
Author(s):  
Thomas Klähn ◽  
David B. Blaschke
Keyword(s):  
Quark Matter ◽  
Strange Quark ◽  
Chiral Symmetry Breaking ◽  
Dense Matter ◽  
Strange Quark Matter ◽  
Compact Stars ◽  
Hadronic Matter ◽  
Model Description ◽  
Severe Problem ◽  
Strange Matter

We discuss possible scenarios for the existence of strange matter in compact stars. The appearance of hyperons leads to a hyperon puzzle in ab-initio approaches based on effective baryon-baryon potentials but is not a severe problem in relativistic mean field models. In general, the puzzle can be resolved in a natural way if hadronic matter gets stiffened at supersaturation densities, an effect based on the quark Pauli quenching between hadrons. We explain the conflict between the necessity to implement dynamical chiral symmetry breaking into a model description and the conditions for the appearance of absolutely stable strange quark matter that require both, approximately masslessness of quarks and a mechanism of confinement. The role of strangeness in compact stars (hadronic or quark matter realizations) remains unsettled. It is not excluded that strangeness plays no role in compact stars at all. To answer the question whether the case of absolutely stable strange quark matter can be excluded on theoretical grounds requires an understanding of dense matter that we have not yet reached.

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