Kaon Condensation in the Neutron Star with a Quark-Meson Coupling Model

2011 ◽  
Vol 59 (2(3)) ◽  
pp. 2114-2117
Author(s):  
C. H. Hyun
Keyword(s):  
Neutron Star ◽  
Coupling Model ◽  
Kaon Condensation ◽  
Meson Coupling

THE STRUCTURE OF NEUTRON STAR BY USING THE QUARK-MESON COUPLING MODEL

2011 ◽  
Vol 01 ◽  
pp. 177-182
Author(s):  
C. Y. RYU ◽  
MYUNG-KI CHEOUN
Keyword(s):  
Neutron Star ◽  
Quark Matter ◽  
Coupling Model ◽  
Bag Model ◽  
Kaon Condensation ◽  
Meson Coupling ◽  
Mit Bag Model

We investigate the structure of neutron star within the framework of the quark-meson coupling model, considering hyperons and kaon condensation. In order to compare the EoS with that from quark matter, the MIT bag model is used. We calculate the mass and radius of a neutron star by using Tolman-Oppenheimer-Volkov equations.

scholarly journals Quark-meson coupling model, nuclear matter constraints, and neutron star properties

2014 ◽  
Vol 89 (6) ◽  
Author(s):  
D. L. Whittenbury ◽  
J. D. Carroll ◽  
A. W. Thomas ◽  
K. Tsushima ◽  
J. R. Stone
Keyword(s):  
Neutron Star ◽  
Nuclear Matter ◽  
Coupling Model ◽  
Meson Coupling

scholarly journals Neutron stars from crust to core within the Quark-meson coupling model

2020 ◽  
Vol 232 ◽  
pp. 03001
Author(s):  
S. Antić ◽  
J. R. Stone ◽  
A. W. Thomas
Keyword(s):  
Neutron Star ◽  
Dense Matter ◽  
Building Blocks ◽  
Coupling Model ◽  
Meson Coupling ◽  
Exciting Time ◽  
Cold Dense Matter ◽  
Finite Nuclei ◽  
Outer Crust

Recent years continue to be an exciting time for the neutron star physics, providing many new observations and insights to these natural ‘laboratories’ of cold dense matter. To describe them, there are many models on the market but still none that would reproduce all observed and experimental data. The quark-meson coupling model stands out with its natural inclusion of hyperons as dense matter building blocks, and fewer parameters necessary to obtain the nuclear matter equation of state. The latest advances of the QMC model and its application to the neutron star physics will be presented, within which we build the neutron star’s outer crust from finite nuclei up to the neutron drip line. The appearance of different elements and their position in the crust of a neutron star is explored and compared to the predictions of various models, giving the same quality of the results for the QMC model as for the models when the nucleon structure is not taken into account.

scholarly journals Neutron Star Properties in the Chiral Quark–Meson Coupling Model

2013 ◽  
Vol 54 (7-10) ◽  
pp. 1591-1594 ◽  
Author(s):  
Tsuyoshi Miyatsu ◽  
Koichi Saito
Keyword(s):  
Neutron Star ◽  
Coupling Model ◽  
Meson Coupling

scholarly journals Neutron star properties in the quark-meson coupling model

1999 ◽  
Vol 60 (1) ◽  
Author(s):  
S. Pal ◽  
M. Hanauske ◽  
I. Zakout ◽  
H. Stöcker ◽  
W. Greiner
Keyword(s):  
Neutron Star ◽  
Coupling Model ◽  
Meson Coupling

scholarly journals δ MESON EFFECTS ON NEUTRON STARS IN THE MODIFIED QUARK–MESON COUPLING MODEL

2010 ◽  
Vol 19 (11) ◽  
pp. 2247-2263 ◽  
Author(s):  
ZHONG-MING NIU ◽  
CHUN-YUAN GAO
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Coupling Model ◽  
Considerable Change ◽  
Hadronic Matter ◽  
Maximum Mass ◽  
Meson Field ◽  
Meson Coupling

The properties of neutron stars are investigated by including δ meson field in the modified quark–meson coupling model. It is found that δ meson has opposite effects on hadronic matter with or without hyperons: it softens the EOSs of hadronic matter with hyperons, while it stiffens the EOSs of pure nucleonic matter. Moreover, by replacing the isovector mesons with the contact scalar–isovector interaction, a considerable change of proton fraction is observed. It is shown that the contact scalar–isovector interaction provides an approach to satisfy the constraint of Direct Urca critical star masses. However, the inclusion of δ meson increases the proton fraction, consequently it decreases the M DU which departs farther from the Direct Urca constraint. Furthermore, the inclusion of δ meson field can increase the maximum mass of neutron star and enlarge the corresponding radius, while these quantities are decreased when the contact scalar–isovector interaction is included.

scholarly journals Outer crust of a cold, nonaccreting neutron star within the quark-meson-coupling model

2020 ◽  
Vol 102 (6) ◽  
Author(s):  
S. Antić ◽  
J. R. Stone ◽  
J. C. Miller ◽  
K. L. Martinez ◽  
P. A. M. Guichon ◽  
...  
Keyword(s):  
Neutron Star ◽  
Coupling Model ◽  
Meson Coupling ◽  
Outer Crust
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