The Structure of Cold Neutron Star With a Quark Core Within the MIT and NJL Models

The Structure of Cold Neutron Star With a Quark Core Within the MIT and NJL Models

Neutron stars due to their high interior matter density are expected to be composed of a quark core, a mixed quark–hadron matter and a layer of hadronic matter. Thus, in this paper, we compute the equation of state of these parts of neutron star to evaluate its structure properties. We use two model...

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Bibliographic Details
Published in:Iranian journal of science and technology. Transaction A, Science Vol. 43; no. 5; pp. 2691 - 2698
Main Authors: Yazdizadeh, T., Bordbar, G. H.
Format: Journal Article
Language:English
Published: Cham Springer International Publishing 01-10-2019
Subjects:
Chemistry/Food Science
Earth Sciences
Engineering
Life Sciences
Materials Science
Physics
Research Paper
NJL model
Quark matter MIT bag model
Radius
Neutron star
Gravitational mass
Quark core
Online Access:Get full text
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Summary:Neutron stars due to their high interior matter density are expected to be composed of a quark core, a mixed quark–hadron matter and a layer of hadronic matter. Thus, in this paper, we compute the equation of state of these parts of neutron star to evaluate its structure properties. We use two models for describing EOS of quark matter, NJL and MIT bag models, and employ three approaches in this work. A density-dependent bag constant satisfies the quark confinement in the simple MIT bag model. We also study the interaction behavior of quarks, firstly one gluon exchange within MIT bag model and the secondly dynamical mass will be held as effective interaction that roles between particles. Density dependence of quark mass is obtained from NJL self-consistent model. NJL model is a effective manner for justifying the chiral symmetry. Applying the Gibbs conditions, the equation of state of the quarks and hadrons mixed phase is obtained. Since the hadronic matter is under the influence of strong force of nucleons, we calculate the equation of state of this phase using a powerful variational many-body technique. Finally, we calculate the mass and radius of a cold neutron star with a quark core by numerically solving the TOV equation. To check our used EOS, we compare our results with the recent observational data. Our results are in a good agreement with some observed compact objects such as S A X J 1748.9 - 2021 , 4 U 1608 - 52 and V e l a X - 1 .
ISSN:1028-6276
2364-1819
DOI:10.1007/s40995-019-00731-3