Isospin properties in quark matter and quark stars within isospin-dependent quark mass models

2019 ◽  
Vol 99 (3) ◽  
Author(s):  
Peng-Cheng Chu ◽  
Yi Zhou ◽  
Xin Qi ◽  
Xiao-Hua Li ◽  
Zhen Zhang ◽  
...  
Keyword(s):  
Quark Matter ◽  
Quark Mass ◽  
Quark Stars

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 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).

scholarly journals Gluon condensates, quark matter equation of state and quark stars

1994 ◽  
Vol 63 (4) ◽  
pp. 681-688 ◽  
Author(s):  
A. Mishra ◽  
H. Mishra ◽  
P. K. Panda ◽  
S. P. Misra
Keyword(s):  
Equation Of State ◽  
Quark Matter ◽  
Quark Stars ◽  
Gluon Condensates

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 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 Thermal conductivity of the quark matter for the SU(2) light-flavor sector

2015 ◽  
Vol 30 (10) ◽  
pp. 1550054 ◽  
Author(s):  
Seung-il Nam
Keyword(s):  
Thermal Conductivity ◽  
Quark Matter ◽  
Quark Mass ◽  
Chemical Potential ◽  
Entropy Density ◽  
Model Parameters ◽  
Chiral Phase ◽  
Nuclear Matter Density ◽  
Wide Range ◽  
Monotonically Decreasing Function

We investigate the thermal conductivity (κ) of the quark matter at finite quark chemical potential (μ) and temperature (T), employing the Green–Kubo formula, for the SU(2) light-flavor sector with the finite current-quark mass m = 5 MeV . As a theoretical framework, we construct an effective thermodynamic potential from the (μ, T)-modified liquid-instanton model (mLIM). Note that all the relevant model parameters are designated as functions of T, using the trivial-holonomy caloron solution. By solving the self-consistent equation of mLIM, we acquire the constituent-quark mass M0 as a function of T and μ, satisfying the universal-class patterns of the chiral phase transition. From the numerical results for κ, we observe that there emerges a peak at μ≈200 MeV for the low-T region, i.e. T≲100 MeV . As T increase over T≈100 MeV , the curve for κ is almost saturated as a function of T in the order of ~ 10-1 GeV 2, and grows with respect to μ smoothly. At the normal nuclear-matter density ρ0 = 0.17 fm -3, κ shows its maximum 6.22 GeV 2 at T≈10 MeV , then decreases exponentially down to κ≈0.2 GeV 2. We also compute the ratio of κ and the entropy density, i.e. κ/s as a function of (μ, T) which is a monotonically decreasing function for a wide range of T, then approaches a lower bound at very high T: κ/s min ≳0.3 GeV -1 in the vicinity of μ = 0.

STABILITY OF QUARK MATTER AND QUARK STARS

2003 ◽  
Author(s):  
M. FIOLHAIS ◽  
M. MALHEIRO ◽  
A. R. TAURINES
Keyword(s):  
Quark Matter ◽  
Quark Stars
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