scholarly journals Strange quark stars within proper time regularized ( 2+1 )-flavor NJL model

2020 ◽  
Vol 101 (6) ◽  
Author(s):  
Cheng-Ming Li ◽  
Shu-Yu Zuo ◽  
Yan Yan ◽  
Ya-Peng Zhao ◽  
Fei Wang ◽  
...  
Keyword(s):  
Strange Quark ◽  
Proper Time ◽  
Quark Stars ◽  
Njl Model

Conversion of neutron stars to 2 + 1 flavor Nambu–Jona-Lasinio quark stars as a mechanism for gamma-ray bursts

2017 ◽  
Vol 32 (37) ◽  
pp. 1750209
Author(s):  
Xiao-Yu Shu ◽  
Yong-Feng Huang ◽  
Hong-Shi Zong
Keyword(s):  
Phase Transition ◽  
Gamma Ray ◽  
Chemical Potential ◽  
Proper Time ◽  
Mean Field ◽  
Gamma Ray Bursts ◽  
Compact Stars ◽  
Relativistic Mean Field ◽  
Quark Stars ◽  
Njl Model

The phase transition from a neutron star to a quark star and its relation to gamma-ray bursts are investigated. A new model: the 2 + 1 flavor Nambu–Jona-Lasinio (NJL) model with the method of proper-time regularization (PTR) is utilized for the quark phase; while the Relativistic Mean Field (RMF) theory is used for the hadronic phase. The process of phase transition is studied by considering the chemical potential, paying special attention to the phase transition point and the emergence of strange quark matter. Characteristics of compact stars are illustrated, and the energy release during the phase transition is found to be [Formula: see text] erg.

scholarly journals Structure of Hot Strange Quark Stars: an NJL Model Approach at Finite Temperature

Astrophysics ◽  
2019 ◽  
Vol 62 (2) ◽  
pp. 276-290 ◽  
Author(s):  
G. H. Bordbar ◽  
R. Hosseini ◽  
F. Kayanikhoo ◽  
A. Poostforush
Keyword(s):  
Finite Temperature ◽  
Strange Quark ◽  
Quark Stars ◽  
Njl Model ◽  
Model Approach

scholarly journals Nonstrange quark stars from an NJL model with proper-time regularization

2019 ◽  
Vol 100 (12) ◽  
Author(s):  
Qingwu Wang ◽  
Chao Shi ◽  
Hong-Shi Zong
Keyword(s):  
Proper Time ◽  
Quark Stars ◽  
Njl Model

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).

Studies on proper time regularization and the QCD chiral phase transition

2019 ◽  
Vol 34 (01) ◽  
pp. 1950003
Author(s):  
Yu-Qiang Cui ◽  
Zhong-Liang Pan
Keyword(s):  
Phase Transition ◽  
Small Parameter ◽  
Effective Mass ◽  
Finite Temperature ◽  
Chemical Potential ◽  
Proper Time ◽  
Chiral Phase ◽  
Chiral Phase Transition ◽  
Njl Model ◽  
The Difference

We investigate the finite-temperature and zero quark chemical potential QCD chiral phase transition of strongly interacting matter within the two-flavor Nambu–Jona-Lasinio (NJL) model as well as the proper time regularization. We use two different regularization processes, as discussed in Refs. 36 and 37, separately, to discuss how the effective mass M varies with the temperature T. Based on the calculation, we find that the M of both regularization schemes decreases when T increases. However, for three different parameter sets, quite different behaviors will show up. The results obtained by the method in Ref. 36 are very close to each other, but those in Ref. 37 are getting farther and farther from each other. This means that although the method in Ref. 37 seems physically more reasonable, it loses the advantage in Ref. 36 of a small parameter dependence. In addition, we also, find that two regularization schemes provide similar results when T [Formula: see text] 100 MeV, while when T is larger than 100 MeV, the difference becomes obvious: the M calculated by the method in Ref. 36 decreases more rapidly than that in Ref. 37.

Population Synthesis of Neutron Stars, Strange (Quark) Stars, and Black Holes

2002 ◽  
Vol 567 (1) ◽  
pp. L63-L66 ◽  
Author(s):  
Krzysztof Belczynski ◽  
Tomasz Bulik ◽  
Włodzimierz Kluźniak
Keyword(s):  
Black Holes ◽  
Neutron Stars ◽  
Strange Quark ◽  
Population Synthesis ◽  
Quark Stars

scholarly journals Effects of Anisotropy on Strongly Magnetized Neutron and Strange Quark Stars in General Relativity

2021 ◽  
Vol 922 (2) ◽  
pp. 149
Author(s):  
Debabrata Deb ◽  
Banibrata Mukhopadhyay ◽  
Fridolin Weber
Keyword(s):  
Magnetic Field ◽  
Field Strength ◽  
Strange Quark ◽  
Radial Direction ◽  
Hydrostatic Equilibrium ◽  
Transverse Orientation ◽  
Quark Stars ◽  
Anisotropic Force ◽  
Local Magnetic Fields ◽  
The Magnetic Field

Abstract We investigate the properties of anisotropic, spherically symmetric compact stars, especially neutron stars (NSs) and strange quark stars (SQSs), made of strongly magnetized matter. The NSs are described by the SLy equation of state (EOS) and the SQSs by an EOS based on the MIT Bag model. The stellar models are based on an a priori assumed density dependence of the magnetic field and thus anisotropy. Our study shows that not only the presence of a strong magnetic field and anisotropy, but also the orientation of the magnetic field itself, have an important influence on the physical properties of stars. Two possible magnetic field orientations are considered: a radial orientation where the local magnetic fields point in the radial direction, and a transverse orientation, where the local magnetic fields are perpendicular to the radial direction. Interestingly, we find that for a transverse orientation of the magnetic field, the stars become more massive with increasing anisotropy and magnetic-field strength and increase in size since the repulsive, effective anisotropic force increases in this case. In the case of a radially oriented magnetic field, however, the masses and radii of the stars decrease with increasing magnetic-field strength because of the decreasing effective anisotropic force. Importantly, we also show that in order to achieve hydrostatic equilibrium configurations of magnetized matter, it is essential to account for both the local anisotropy effects as well as the anisotropy effects caused by a strong magnetic field. Otherwise, hydrostatic equilibrium is not achieved for magnetized stellar models.

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