The equation of state (EoS) of a hot proto-neutron star matter with trapped neutrinos was calculated within the effective SU(3) theory with the enhanced vector meson sector
The true nature and the internal constitution of the compact stars known as neutron stars (NSs) is o...
Analysis of the density dependence of the symmetry energy in the case of strangeness-rich neutron s...
This paper gives an overview of the model of a neutron star with non-zero strangeness constructed wi...
The analysis based on the relativistic mean field (RMF) theory with the isoscalar–isovector interact...
The linear chiral SU(3)L×SU(3)R model is applied to describe properties of the compact star matter i...
We investigate various properties of neutron star matter within an e ective chiral SU(3)L × SU(3)R m...
A proto-neutron star (PNS) is the first phase of life of a neutron star, and is likely to origin fro...
The true nature and the internal constitution of the compact stars known as neutron stars (NSs) is o...
Relativistic mean field (RMF) theory of nuclear matter with the isovector scalar mean field correspo...
In this work we present a detailed explanation of the construction of an appropriate equation of sta...
The equation of state of asymmetric nuclear matter given by the parameterized form of the relativist...
Understanding the properties of dense matter is one of the most outstanding challenges in nuclear (a...
In this thesis, we first investigated the effect of Lambda pairing on the ground state properties of...
In the first part of this paper, we use a nonlocal extension of the three-flavor Polyakov-Nambu-Jona...
Neutron stars are like nuclear physics laboratories, providing a unique opportunity to apply and sea...
The true nature and the internal constitution of the compact stars known as neutron stars (NSs) is o...
Analysis of the density dependence of the symmetry energy in the case of strangeness-rich neutron s...
This paper gives an overview of the model of a neutron star with non-zero strangeness constructed wi...
The analysis based on the relativistic mean field (RMF) theory with the isoscalar–isovector interact...
The linear chiral SU(3)L×SU(3)R model is applied to describe properties of the compact star matter i...
We investigate various properties of neutron star matter within an e ective chiral SU(3)L × SU(3)R m...
A proto-neutron star (PNS) is the first phase of life of a neutron star, and is likely to origin fro...
The true nature and the internal constitution of the compact stars known as neutron stars (NSs) is o...
Relativistic mean field (RMF) theory of nuclear matter with the isovector scalar mean field correspo...
In this work we present a detailed explanation of the construction of an appropriate equation of sta...
The equation of state of asymmetric nuclear matter given by the parameterized form of the relativist...
Understanding the properties of dense matter is one of the most outstanding challenges in nuclear (a...
In this thesis, we first investigated the effect of Lambda pairing on the ground state properties of...
In the first part of this paper, we use a nonlocal extension of the three-flavor Polyakov-Nambu-Jona...
Neutron stars are like nuclear physics laboratories, providing a unique opportunity to apply and sea...
The true nature and the internal constitution of the compact stars known as neutron stars (NSs) is o...
Analysis of the density dependence of the symmetry energy in the case of strangeness-rich neutron s...
This paper gives an overview of the model of a neutron star with non-zero strangeness constructed wi...
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