Abstract
Motivated by importance of the existence of quark matter on structure of neutron star. For this purpose, we use a suitable equation of state (EoS) which include three different parts: (i) a layer of hadronic matter, (ii) a mixed phase of quarks and hadrons, and, (iii) a strange quark matter in the core. For this system, in order to do more investigation of the EoS, we evaluate energy, Le Chatelier’s principle and stability conditions. Our results show that the EoS satisfies these conditions. Considering this EoS, we study the effect of quark matter on the structure of neutron stars such as maximum mass and the corresponding radius, average density, compactness, Kretschmann scalar, Schwarzschild radius, gravitational redshift and dynamical stability. Also, considering the mentioned EoS in this paper, we find that the maximum mass of hybrid stars is a little smaller than that of the corresponding pure neutron star. Indeed the maximum mass of hybrid stars can be quite close to the pure neutron stars. Our calculations about the dynamical stability show that these stars are stable against the radial adiabatic infinitesimal perturbations. In addition, our analyze indicates that neutron stars are under a contraction due to the existence of quark core.
Highlights
Considering this equation of state (EoS), we study the effect of quark matter on the structure of neutron stars such as maximum mass and the corresponding radius, average density, compactness, Kretschmann scalar, Schwarzschild radius, gravitational redshift and dynamical stability
The paper at hand studied the structure of cold hybrid stars which included three different parts: (i) a layer of hadronic matter, (ii) a mixed phase of quarks and hadrons, and (iii) a quark matter in the core
Our results indicated that the maximum mass, the average density, compactness, gravitational redshift, and Kretschmann scalar of neutron stars decrease by adding a quark core to them
Summary
In order to study the structure of stars and their phenomenological properties, we must use the hydrostatic equilibrium equation (HEE). In order to evaluate a suitable EoS, we will study energy, Le Chatelier’s principle and stability conditions of this EoS Another our goal is related to the investigation of the effects of quark core in the structure of hybrid star. We compare the structure of neutron stars by considering the EoS with and without a quark core. It should be noted that for calculation of the structure properties of neutron star, the equation of state of hadronic matter has a crucial role. For the hadronic matter calculations, we use the U V 14 + T N I potential in which the effect of three-body nuclear force has been considered
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