QUARK STARS IN CHIRAL COLOR DIELECTRIC MODEL

1993 ◽  
Vol 02 (03) ◽  
pp. 575-586 ◽  
Author(s):  
SANJAY K. GHOSH ◽  
PRADIP K. SAHU
Keyword(s):  
Equation Of State ◽  
Quark Matter ◽  
Thermodynamic Potential ◽  
Interaction Strength ◽  
Expectation Value ◽  
Quark Masses ◽  
Quark Stars ◽  
Dielectric Model ◽  
Interaction Term ◽  
Gluon Interaction

The nonlinear chiral extension of color dielectric model has been used in the present work to study the properties of quark stars. Assuming that the square of meson fields develops nonzero expectation value, the thermodynamic potential for charge neutral interacting two- and three-flavor quark matter, in beta equilibrium, has been calculated up to second order in quark gluon interaction term in the Lagrangian. The equation of state has been found to be softer for higher quark masses and interaction strength. The quark stars properties are found to be dependent on EOS. The mass, radius, moment of inertia and gravitational red shift decrease as the equation of state becomes more soft.

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

scholarly journals Hybrid stars from a three-flavor NJL model with two kinds of tensor condensates

2020 ◽  
Vol 29 (10) ◽  
pp. 2050093
Author(s):  
Masatoshi Morimoto ◽  
Yasuhiko Tsue ◽  
João da Providência ◽  
Constança Providência ◽  
Masatoshi Yamamura
Keyword(s):  
Equation Of State ◽  
Quark Matter ◽  
Thermodynamic Potential ◽  
Chemical Potential ◽  
Point Interaction ◽  
Condensed Phases ◽  
Charge Neutrality ◽  
Njl Model ◽  
Hybrid Stars ◽  
The Relationship

To obtain the equation of state of quark matter and construct hybrid stars, we calculate the thermodynamic potential in the three-flavor Nambu–Jona-Lasinio model including the tensor-type four-point interaction and the Kobayashi–Maskawa–’t Hooft interaction. To construct the hybrid stars, it is necessary to impose the [Formula: see text] equilibrium and charge neutrality conditions on the system. It is shown that tensor condensed phases appear at large chemical potential. Under the possibility of the existence of the tensor condensates, the relationship between the radius and mass of hybrid stars is estimated.

scholarly journals ANALYTICAL MODELS FOR QUARK STARS

2007 ◽  
Vol 16 (11) ◽  
pp. 1803-1811 ◽  
Author(s):  
K. KOMATHIRAJ ◽  
S. D. MAHARAJ
Keyword(s):  
Electromagnetic Field ◽  
Equation Of State ◽  
Exact Solutions ◽  
Quark Matter ◽  
Matter Content ◽  
Analytical Models ◽  
System Of Equations ◽  
Maxwell System ◽  
Elementary Functions ◽  
Quark Stars

We find two new classes of exact solutions to the Einstein–Maxwell system of equations. The matter content satisfies a linear equation of state consistent with quark matter; a particular form of one of the gravitational potentials is specified to generate solutions. The exact solutions can be written in terms of elementary functions, and these can be related to quark matter in the presence of an electromagnetic field. The first class of solutions generalizes the Mak–Harko model. The second class of solutions does not admit any singularities in the matter and gravitational potentials at the center.

QUARK MATTER IN NEUTRON STARS: AN APERÇU

2006 ◽  
Vol 21 (26) ◽  
pp. 1965-1979 ◽  
Author(s):  
PRASHANTH JAIKUMAR ◽  
SANJAY REDDY ◽  
ANDREW W. STEINER
Keyword(s):  
Neutron Star ◽  
Equation Of State ◽  
Neutron Stars ◽  
Quark Matter ◽  
Finite Size ◽  
Coulomb Energy ◽  
Quark Stars ◽  
Dense Quark Matter ◽  
Intermediate Fraction ◽  
State Of Matter

The existence of deconfined quark matter in the superdense interior of neutron stars is a key question that has drawn considerable attention over the past few decades. Quark matter can comprise an arbitrary fraction of the star, from 0 for a pure neutron star to 1 for a pure quark star, depending on the equation of state of matter at high density. From an astrophysical viewpoint, these two extreme cases are generally expected to manifest different observational signatures. An intermediate fraction implies a hybrid star, where the interior consists of mixed or homogeneous phases of quark and nuclear matter, depending on surface and Coulomb energy costs, as well as other finite size and screening effects. In this review, we discuss what we can deduce about quark matter in neutron stars in light of recent exciting developments in neutron star observations. We state the theoretical ideas underlying the equation of state of dense quark matter, including color superconducting quark matter. We also highlight recent advances stemming from re-examination of an old paradigm for the surface structure of quark stars and discuss possible evolutionary scenarios from neutron stars to quark stars, with emphasis on astrophysical observations.

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).

Algorithms for Density, Potential Temperature, Conservative Temperature, and the Freezing Temperature of Seawater

2006 ◽  
Vol 23 (12) ◽  
pp. 1709-1728 ◽  
Author(s):  
David R. Jackett ◽  
Trevor J. McDougall ◽  
Rainer Feistel ◽  
Daniel G. Wright ◽  
Stephen M. Griffies
Keyword(s):  
Thermal Expansion ◽  
Equation Of State ◽  
Thermodynamic Potential ◽  
Potential Temperature ◽  
Inverse Function ◽  
Freezing Temperature ◽  
Ocean Models ◽  
The Difference ◽  
New Equation ◽  
Density Equation

Abstract Algorithms are presented for density, potential temperature, conservative temperature, and the freezing temperature of seawater. The algorithms for potential temperature and density (in terms of potential temperature) are updates to routines recently published by McDougall et al., while the algorithms involving conservative temperature and the freezing temperatures of seawater are new. The McDougall et al. algorithms were based on the thermodynamic potential of Feistel and Hagen; the algorithms in this study are all based on the “new extended Gibbs thermodynamic potential of seawater” of Feistel. The algorithm for the computation of density in terms of salinity, pressure, and conservative temperature produces errors in density and in the corresponding thermal expansion coefficient of the same order as errors for the density equation using potential temperature, both being twice as accurate as the International Equation of State when compared with Feistel’s new equation of state. An inverse function relating potential temperature to conservative temperature is also provided. The difference between practical salinity and absolute salinity is discussed, and it is shown that the present practice of essentially ignoring the difference between these two different salinities is unlikely to cause significant errors in ocean models.

scholarly journals Mass distribution from a quark matter equation of state

2007 ◽  
Vol 75 (3) ◽  
Author(s):  
T. S. Biró ◽  
P. Lévai ◽  
P. Ván ◽  
J. Zimányi
Keyword(s):  
Equation Of State ◽  
Mass Distribution ◽  
Quark Matter

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
Sign in / Sign up

Export Citation Format

Share Document