Abstract
The nuclear symmetry energy is a quantity especially important for neutron stars as it is directly related to the nuclear matter equation of state (EoS), which, in turn, unambiguously determines the EoS of the uniform neutron star matter. Neutron star matter is characterized by a high value of the neutron–proton asymmetry, which is settled by the β-equilibrium condition. At sufficiently high density relevant for the inner core of a neutron star the equilibrium conditions predict the appearance of additional degrees of freedom with hyperons as the most obvious candidates, thus it is expected that symmetry energy being encoded in the EoS of strangeness-rich nuclear matter influences many properties of neutron stars. Experimental determination of the symmetry energy is beset by problems that are connected with the fact that the symmetry energy is not a physical observable and the only experimentally accessible information comes from indirect measurements [1].
Highlights
The nuclear symmetry energy is a quantity especially important for neutron stars as it is directly related to the nuclear matter equation of state (EoS), which, in turn, unambiguously determines the EoS of the uniform neutron star matter
Neutron star matter is characterized by a high value of the neutron–proton asymmetry, which is settled by the β-equilibrium condition
The density dependence of the binding energy was calculated for the asymmetric nuclear matter in the case of weak model (WEAK), when strange mesons are introduced in the minimal fashion, and nonlinear extended model (EXT), for the neutron–proton asymmetry δa = 0.5 and for the parameter ΛV = 0.0165
Summary
The nuclear symmetry energy is a quantity especially important for neutron stars as it is directly related to the nuclear matter equation of state (EoS), which, in turn, unambiguously determines the EoS of the uniform neutron star matter. Neutron star matter is characterized by a high value of the neutron–proton asymmetry, which is settled by the β-equilibrium condition. At sufficiently high density relevant for the inner core of a neutron star the equilibrium conditions predict the appearance of additional degrees of freedom with hyperons as the most obvious candidates, it is expected that symmetry energy being encoded in the EoS of strangeness-rich nuclear matter influences many properties of neutron stars. Experimental determination of the symmetry energy is beset by problems that are connected with the fact that the symmetry energy is not a physical observable and the only experimentally accessible information comes from indirect measurements [1]
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