We study the effects of symmetry energy on neutron drip density and properties nuclei in star crusts. The nonuniform matter around point is calculated by using Thomas--Fermi approximation with relativistic mean-field model. composition crust are found to be correlated its slope. compare self-consistent other treatments surface Coulomb energies find that these finite-size play an essential role determining equilibrium state at low density.

We investigate the effects of symmetry energy on nuclear pasta phases and crust-core transition in neutron stars. employ relativistic mean-field approach coexisting method to study properties presented inner crust It is found that slope at saturation density plays an important role phase properties. The correlation between obtained this consistent with those by other methods.

We study the impact of symmetry energy on properties nuclear pasta phases and crust-core transition in neutron stars. perform a self-consistent Thomas-Fermi calculation employing relativistic mean-field model. The presented inner crust stars are investigated is examined. It found that slope plays an important role determining phase structure transition. correlation between density obtained approximation consistent with predicted by liquid-drop

We study the effects of nuclear symmetry energy on mass-radius relation and tidal deformability neutron stars, considering self-consistency equation state (EOS). first construct a set unified EOSs based relativistic mean-field models with different density dependence energy. For description pasta phases appearing in inner crust we perform self-consistent Thomas-Fermi calculation using same interaction as that for uniform matter core. To examine possible from EOS neutron-star properties,...

Abstract The radii and tidal deformabilities of neutron stars are investigated in the framework relativistic mean-field (RMF) model with different density-dependent behaviors symmetry energy. To study effects energy on properties stars, $\omega$ meson $\rho$ coupling terms included a popular RMF Lagrangian, i.e., TM1 parameter set, which is adopted for widely used supernova equation state (EoS) table. constants relevant to vector–isovector meson, $\rho$, refitted by fixed at subsaturation...

The secondary component of GW190814 with a mass 2.50-2.67 $M_{\odot}$ may be the lightest black hole or heaviest neutron star ever observed in binary compact object system. To explore possible equation state (EOS), which can support such massive star, we apply relativistic mean-field model density-dependent isovector coupling constant to describe neutron-star matter. acceptable EOS should satisfy some constraints: provide satisfactory description nuclei; maximum $M_\textrm{TOV}$ is above 2.6...

We develop a self-consistent description of hot nuclei within the relativistic Thomas--Fermi approximation using mean-field model for nuclear interactions. The temperature dependence symmetry energy and other physical quantities nucleus are calculated by employing subtraction procedure in order to isolate from surrounding nucleon gas. It is found that coefficient finite significantly affected Coulomb polarization effect. also examine results on interactions make comparison between obtained...

We study the liquid-gas phase transition of stellar matter with inclusion finite-size effect from surface and Coulomb energies. The equilibrium conditions for two coexisting phases are determined by minimizing total free energy including contributions, which different Gibbs used in bulk calculations. can significantly reduce region mixed phase. influence symmetry on is investigated effects. It found that slope plays an important role determining boundary properties

We study the impact of strong magnetic fields on pasta phases that are expected to exist in inner crust neutron stars. employ relativistic mean field model describe nucleon interaction and use self-consistent Thomas-Fermi approximation calculate nonuniform matter star crust. The properties crust-core transition examined. It is found as strength $B$ less than $10^{17}$ G, effects not evident comparing with results without field. As stronger $10^{18}$ onset densities density decrease...

We explore the properties of nuclear pasta appearing in supernova matter, i.e., matter at finite temperature with a fixed proton fraction. The phases series geometric shapes are studied using compressible liquid-drop (CLD) model, where separates into dense liquid phase nucleons and dilute gas $\ensuremath{\alpha}$ particles. equilibrium conditions for two coexisting derived by minimization total free energy including surface Coulomb contributions, which clearly different from Gibbs due to...

A self-consistent description for hot $\Lambda$ hypernuclei in hypothetical big boxes is developed within the relativistic Thomas-Fermi approximation order to investigate directly liquid-gas phase coexistence strangeness finite nuclear systems. We use mean-field model interactions. The temperature dependence of hyperon density, radius, excitation energies, specific heat, and binding energies from $^{16}_{\Lambda}$O $^{208}_{\Lambda}$Pb transition region are calculated by using subtraction...

It is generally believed that a neutron star mainly consists of four parts,that to say, outer crust, inner core, and core.From drip density crust-core transition density,the crust nonuniform system wherenuclei coexist with nucleon electron gases surrounding them.As increases, the nuclear pasta phases different shapes,such as droplet, rod, slab, tube, bubble may appear in crust.Astronomical observations indicate strong magnetic fields, which be high 10$^{18}$ G, exist some stars.So, structure...

We study the impact of symmetry energy on properties nuclear pasta phases and crust-core transition in neutron stars. perform a self-consistent Thomas--Fermi calculation employing relativistic mean-field model. The presented inner crust stars are investigated is examined. It found that slope plays an important role determining phase structure transition. correlation between density obtained approximation consistent with predicted by liquid-drop

Using the relativistic mean-field theory, we adopt two different methods, namely, coexisting phase method and self-consistent Thomas-Fermi approximation, to study impacts of nuclear symmetry energy on properties neutron star crusts within a wide range densities. It is found that its density slope play an important role in determining pasta phases crust-core transition.

We study the equations of state nuclear matter and neutron-star matter, which are crucial inputs for supernova calculations.We employ relativistic mean-field model to describe interactions.The phase transition from nonuniform uniform is determined in a consistent manner.The deconfinement at high densities examined using equilibrium conditions derived by minimization total free energy.

The radii and tidal deformabilities of neutron stars are investigated in the framework relativistic mean-field (RMF) model with different density-dependent behaviors symmetry energy. To study effects energy on properties stars, an $\omega$ meson $\rho$ coupling term is included a popular RMF Lagrangian, i.e. TM1 parameter set, which used for widely supernova equation state (EoS) table. constants relevant to vector-isovector meson, $\rho$, refitted by fixed at subsaturation density its slope...