NEUTRON STARS WITH KAON CONDENSATION IN RELATIVISTIC EFFECTIVE MODEL

2013 ◽  
Vol 22 (05) ◽  
pp. 1350026 ◽  
Author(s):  
CHEN WU ◽  
WEI-LIANG QIAN ◽  
YU-GANG MA ◽  
JI-FENG YANG
Keyword(s):  
Field Theory ◽  
Neutron Star ◽  
Neutron Stars ◽  
Nuclear Matter ◽  
Optical Potential ◽  
Mean Field Theory ◽  
Mean Field ◽  
Neutron Star Matter ◽  
Relativistic Mean Field ◽  
Kaon Condensation

Relativistic mean-field theory with parameter sets FSUGold and IU-FSU is extended to study the properties of neutron star matter in β equilibrium by including Kaon condensation. The mixed phase of normal baryons and Kaon condensation cannot exist in neutron star matter for the FSUGold model and the IU-FSU model. In addition, it is found that when the optical potential of the K- in normal nuclear matter UK ≳ -100 MeV , the Kaon condensation phase is absent in the inner cores of the neutron stars.

scholarly journals STRUCTURE AND PROPERTIES OF NEUTRON STARS IN THE RELATIVISTIC MEAN-FIELD THEORY

2001 ◽  
Vol 10 (05) ◽  
pp. 607-624 ◽  
Author(s):  
ILONA BEDNAREK ◽  
RYSZARD MANKA
Keyword(s):  
Field Theory ◽  
Neutron Star ◽  
Neutron Stars ◽  
Mean Field Theory ◽  
Mean Field ◽  
Neutron Star Matter ◽  
Relativistic Mean Field Theory ◽  
X Ray ◽  
Relativistic Mean Field ◽  
Bulk Parameters

Properties of rotating neutron stars with the use of relativistic mean-field theory are considered. The performed analysis of neutron star matter is based on the nonlinear Lgrangian density. The presence of nonlinear interaction of vector mesons modifies the density dependence of the ρ field and influences bulk parameters of neutron stars. The observed quasiperiodic X-ray oscillations of low mass X-ray binaries can be used in order to constrain the equation of state of neutron star matter. Having assumed that the maximum frequency of the quasiperiodic oscillations originates at the circular orbit it is possible to estimate masses and radii of neutron stars.

THE EFFECT OF THE SCALAR-ISOVECTOR MESON FIELD ON HYPERON-RICH NEUTRON STAR MATTER

2008 ◽  
Vol 17 (07) ◽  
pp. 1293-1307 ◽  
Author(s):  
AI-JUN MI ◽  
WEI ZUO ◽  
ANG LI
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Mean Field Theory ◽  
Mean Field ◽  
Maximum Mass ◽  
Meson Field ◽  
Neutron Star Matter ◽  
Relativistic Mean Field ◽  
Strangeness Content ◽  
Positively Charged

We investigate the effect of the scalar-isovector δ-meson field on the equation of state (EOS) and composition of hyperonic neutron star matter, and the properties of hyperonic neutron stars within the framework of the relativistic mean field theory. The influence of the δ-field turns out to be quite different and generally weaker for hyperonic neutron star matter as compared to that for npeμ neutron star matter. We find that inclusion of the δ-field enhances the strangeness content slightly and consequently moderately softens the EOS of neutron star matter in its hyperonic phase. As for the composition of hyperonic star matter, the effect of the δ-field is shown to shift the onset of the negatively-charged (positively-charged) hyperons to slightly lower (higher) densities and to enhance (reduce) their abundances. The influence of the δ-field on the maximum mass of hyperonic neutron stars is found to be fairly weak, whereas inclusion of the δ-field turns out to enhance sizably both the radii and the moments of inertia of neutron stars with given masses. It is also shown that the effects of the δ-field on the properties of hyperonic neutron stars remain similar in the case of switching off the Σ hyperons.

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