Nuclear equation of state at high baryonic density and compact star constraints

Abstract

A mean field calculation is carried out to obtain the equation of state (EoS) of nuclear matter from a density dependent M3Y interaction (DDM3Y). The energy per nucleon is minimized to obtain ground state of the symmetric nuclear matter (SNM). The constants of density dependence of the effective interaction are obtained by reproducing the saturation energy per nucleon and the saturation density of SNM. The energy variation of the exchange potential is treated properly in the negative energy domain of nuclear matter. The EoS of SNM, thus obtained, is not only free from the superluminosity problem but also provides excellent estimate of nuclear incompressibility. The EoS of asymmetric nuclear matter is calculated by adding to the isoscalar part, the isovector component of M3Y interaction. The SNM and pure neutron matter EoS are used to calculate the nuclear symmetry energy which is found to be consistent with that extracted from the isospin diffusion in heavy-ion collisions at intermediate energies. The $\beta$ equilibrium proton fraction calculated from the symmetry energy and related theoretical findings are consistent with the constraints derived from the observations on compact stars.

26 pages including 2 tables and 7 figures

References in corpus (11)

• Constraints on the high-density nuclear equation of state from the phenomenology of compact stars and heavy-ion collisions
• Nuclear rainbow scattering and nucleus-nucleus potential
• Alpha decay half-lives of new superheavy elements
• Predictions of Alpha Decay Half lives of Heavy and Superheavy Elements
• Cooling of the quasi-persistent neutron star X-ray transients KS 1731-260 and MXB 1659-29
• Folding model analysis of proton radioactivity of spherical proton emitters
• Alpha decay chains from element 113
• Coefficients and terms of the liquid drop model and mass formula
• Neutron stars and quark matter
• Compact star constraints on the high-density EoS
• The Equation of State of Dense Matter : from Nuclear Collisions to Neutron Stars

Cited by in corpus (12)

• Towards Understanding Astrophysical Effects of Nuclear Symmetry Energy
• Constraining the High-Density Behavior of Nuclear Symmetry Energy with the Tidal Polarizability of Neutron Stars
• Equation of state of the neutron star matter, and the nuclear symmetry energy
• Isospin dependent properties of asymmetric nuclear matter
• Impact of Symmetry Energy on Sound Speed and Spinodal Decomposition in Dense Neutron-Rich Matter
• Cluster radioactivity in very heavy nuclei: a new perspective
• Stability of the $\beta$-equilibrated dense matter and core-crust transition in neutron stars
• Stability against $\alpha$ decay of some recently observed superheavy elements
• From nuclear reactions to compact stars: a unified approach
• Isospin asymmetric nuclear matter and properties of axisymmetric neutron stars
• Folding model analysis of ${}^{12}C{-}^{12}C$ and ${}^{16}O{-}^{16}O$ elastic scattering using the density-dependent LOCV averaged effective interaction
• Density Dependence of Nuclear Symmetry Energy