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Soviet Physics Journal, 1974
The basic parameters — mass and radius — of the quark configurations having central densities from 1019 to 1032 g/cm3 are obtained. It is shown that similar objects should have large gravitational mass defects. The curve of the stable configurations is extended to the region of densities substantially exceeding those of the nucleus.
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The basic parameters — mass and radius — of the quark configurations having central densities from 1019 to 1032 g/cm3 are obtained. It is shown that similar objects should have large gravitational mass defects. The curve of the stable configurations is extended to the region of densities substantially exceeding those of the nucleus.
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Fortschritte der Physik, 1986
AbstractPossible existence of quark‐matter in dense neutron‐stars is discussed using Quantum Chromodynamical equation of state for cold degenerate quark‐matter.
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AbstractPossible existence of quark‐matter in dense neutron‐stars is discussed using Quantum Chromodynamical equation of state for cold degenerate quark‐matter.
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STABILITY OF QUARK MATTER AND QUARK STARS
New Worlds in Astroparticle Physics, 2003We use the confining chromodielectric model to study quark matter. In the version of the model with a quartic potential for the confining field we obtain two solutions for the mean-field equations. The resulting equations of state for strange quark matter are degenerate at large densities with a small energy barrier between them.
M. Malheiro +2 more
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Classical and Quantum Gravity, 1991
The authors calculate the mass, radius, moment of inertia and surface gravitational red shift of quark stars described by three models: the noninteracting Fermi gas model of Itoh (1970), the asymptotic MIT bag model, and the perturbative QCD model of Chapline and Nauenberg (1977). They report the results of phase transition calculations, and comment on
E Ostgaard, T Overgard
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The authors calculate the mass, radius, moment of inertia and surface gravitational red shift of quark stars described by three models: the noninteracting Fermi gas model of Itoh (1970), the asymptotic MIT bag model, and the perturbative QCD model of Chapline and Nauenberg (1977). They report the results of phase transition calculations, and comment on
E Ostgaard, T Overgard
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Physical Review D, 1978
We analyze models of quark matter appropriate to the description of matter at densities found within neutron stars. We consider in detail two models: quantum chromodynamics with a bag constant B = 56 MeV/fm/sup 3/, and quantum chromodynamics with B = 0.
Barry A. Freedman, Larry McLerran
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We analyze models of quark matter appropriate to the description of matter at densities found within neutron stars. We consider in detail two models: quantum chromodynamics with a bag constant B = 56 MeV/fm/sup 3/, and quantum chromodynamics with B = 0.
Barry A. Freedman, Larry McLerran
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2000
We study the relativistic quadrupole oscillations (ι= 2) of strange quark stars by calculating their quasi-normal modes, and we thus explore the possibility of using these oscillation frequencies and damping times to differentiate among relativistic polytropic stars, neutron stars, pure light-quark stars, and hybrid neutron stars with quark cores.
C. W. Yip, Ming Chung Chu, P. T. Leung
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We study the relativistic quadrupole oscillations (ι= 2) of strange quark stars by calculating their quasi-normal modes, and we thus explore the possibility of using these oscillation frequencies and damping times to differentiate among relativistic polytropic stars, neutron stars, pure light-quark stars, and hybrid neutron stars with quark cores.
C. W. Yip, Ming Chung Chu, P. T. Leung
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Coalescence of black hole–neutron star binaries
Living Reviews in Relativity, 2021Koutarou Kyutoku +2 more
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