scholarly journals Radial Oscillations of Quark Stars Admixed with Dark Matter

Universe ◽  
2022 ◽  
Vol 8 (1) ◽  
pp. 34
Author(s):  
José C. Jiménez ◽  
Eduardo S. Fraga
Keyword(s):  
Dark Matter ◽  
Fundamental Frequency ◽  
Quark Matter ◽  
Compact Stars ◽  
Radial Oscillation ◽  
Quark Stars ◽  
Oscillation Frequencies

We investigated compact stars consisting of cold quark matter and fermionic dark matter treated as two admixed fluids. We computed the stellar structures and fundamental radial oscillation frequencies of different masses of the dark fermion in the cases of weak and strong self-interacting dark matter. We found that the fundamental frequency can be dramatically modified and, in some cases, stable dark strange planets and dark strangelets with very low masses and radii can be formed.

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 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 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.

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.

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 Dark Matter, Neutron Stars, and Strange Quark Matter

2010 ◽  
Vol 105 (14) ◽  
Author(s):  
M. Angeles Perez-Garcia ◽  
Joseph Silk ◽  
Jirina R. Stone
Keyword(s):  
Dark Matter ◽  
Neutron Stars ◽  
Quark Matter ◽  
Strange Quark ◽  
Strange Quark Matter

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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