https://www.psi.ir/physics_society_iran_1_homeIranian Journal of Physics Research1682-695721420220220The equilibrium configuration of rotating neutron stars The equilibrium configuration of rotating neutron stars 765774175210.47176/ijpr.21.4.21011 FARRiahiDepartment of Physics, Shahrekord Branch, Islamic Azad University, Shahrekord, IranS ZKalantariDepartment of Physics, Isfahan University of Technology, Isfahan, IranJournal Article20200223Using the density-dependent equation of states to describe the matter of rotating neutron stars, we construct equilibrium configurations of rotating neutron stars. The interaction between baryons is described by exchanging the scalar and vector mesons in the relativistic mean-field theory. The mesons coupling coefficients are functions of the environmental density. The sequence of equilibrium states is calculated for the four frequencies observed for rotating neutron stars namely, 25, 317, 716, and 1122 Hz. These sequences are constrained by static, Keplerian (mass-shedding sequence), and secular axisymmetric instability sequences. This allows the radius and mass range of the stars will be obtained in each of the models. We can also calculate the parameters of the fastest rotating star described by each model.Using the density-dependent equation of states to describe the matter of rotating neutron stars, we construct equilibrium configurations of rotating neutron stars. The interaction between baryons is described by exchanging the scalar and vector mesons in the relativistic mean-field theory. The mesons coupling coefficients are functions of the environmental density. The sequence of equilibrium states is calculated for the four frequencies observed for rotating neutron stars namely, 25, 317, 716, and 1122 Hz. These sequences are constrained by static, Keplerian (mass-shedding sequence), and secular axisymmetric instability sequences. This allows the radius and mass range of the stars will be obtained in each of the models. We can also calculate the parameters of the fastest rotating star described by each model.https://ijpr.iut.ac.ir/article_1752_058f6b585235b58050d529a4aa58501d.pdf