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Exercise capacity and cardiac allograft ischemic time in recent heart transplant recipients. [PDF]
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Stability of Quark Star Models
Communications in Theoretical Physics, 2016Summary: In this paper, we investigate the stability of quark stars with four different types of inner matter configurations; isotropic, charged isotropic, anisotropic and charged anisotropic by using the concept of cracking. For this purpose, we have applied local density perturbations technique to the hydrostatic equilibrium equation as well as on ...
Azam, M., Mardan, S. A., Rehman, M. A.
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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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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. FIOLHAIS, M. MALHEIRO, A. R. TAURINES
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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 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 Freedman, Larry McLerran
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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
T Overgard, E Ostgaard
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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
T Overgard, E Ostgaard
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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, M. C. 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, M. C. Chu, P. T. Leung
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Chinese Journal of Astronomy and Astrophysics, 2006
Members of the family of pulsar-like stars are distinguished by their different manifestations observed, i.e., radio pulsars, accretion-driven X-ray pulsars, X-ray bursts, anomalous X-ray pulsars/soft gamma-ray repeaters, certral compact objects, and dim thermal neutron stars.
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Members of the family of pulsar-like stars are distinguished by their different manifestations observed, i.e., radio pulsars, accretion-driven X-ray pulsars, X-ray bursts, anomalous X-ray pulsars/soft gamma-ray repeaters, certral compact objects, and dim thermal neutron stars.
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