From nuclear reactions to compact stars: A unified approach

Abstract

An equation of state (EoS) for symmetric nuclear matter is constructed using the density dependent M3Y effective interaction and extended for isospin asymmetric nuclear matter. Theoretically obtained values of symmetric nuclear matter incompressibility, isobaric incompressibility, symmetry energy and its slope agree well with experimentally extracted values. Folded microscopic potentials using this effective interaction, whose density dependence is determined from nuclear matter calculations, provide excellent descriptions for proton, alpha and cluster radioactivities, elastic and inelastic scattering. The nuclear deformation parameters extracted from inelastic scattering of protons agree well with other available results. The high density behavior of symmetric and asymmetric nuclear matter satisfies the constraints from the observed flow data of heavy-ion collisions. The neutron star properties studied using β-equilibrated neutron star matter obtained from this effective interaction for pure hadronic model agree with the recent observations of the massive compact stars such as PSR J1614-2230, but if a phase transition to quark matter is considered such agreement is no longer possible.

Nuclear constraints on the core-crust transition and crustal fraction of moment of inertia of neutron stars

“…The single integration constant needed to solve the TOV equation is P c , the pressure at the center of the star calculated at a given central density ρ c . The masses of slowly rotating neutron stars are very close [25][26][27] to those obtained by solving TOV equation.…”

“…In summary, the DDM3Y effective interaction which provides a unified description of elastic and inelastic scattering, proton-, α-, cluster-radioactivities and nuclear matter properties, also provides an excellent description of the β-equilibrated neutron star matter which is stiff enough at high densities to reconcile with the recent ob-servations of the massive compact stars [25][26][27] while the corresponding symmetry energy is supersoft as preferred by the FOPI/GSI experimental data. The neutron star core-crust transition density, pressure and proton fraction determined from the thermodynamic stability condition to be ρ t = 0.0938 fm −3 , P t = 0.5006 MeV fm −3 and x p(t) = 0.0308, respectively, along with observed minimum crustal fraction of the total moment of inertia of the Vela pulsar provide a new limit for its radius.…”

Stability ofβ-equilibrated dense matter and core-crust transition in neutron stars

“…The nucleon-nucleon effective interaction used in the present work, which is found to provide a unified description of elastic and inelastic scattering, various radioactivities and nuclear matter properties, also provides an excellent description of the β-equilibrated neutron star matter which is stiff enough at high densities to reconcile with the recent observations of the massive compact stars [55][56][57] while the corresponding symmetry energy is supersoft as preferred by the FOPI/GSI experimental data. The density, the pressure and the proton fraction at the inner edge separating the liquid core from the solid crust of the neutron stars determined to be ρ t = 0.0938 fm −3 , P t = 0.5006 MeV fm −3 and x p(t) = 0.0308, respectively, are also in close agreement with other theoretical calculations [54] corresponding to high nuclear incompressibility and with those obtained using SLy4 interaction [58].…”

Effect of the DDM3Y Nuclear Equation of State on the R-mode Instability of Neutron Stars

“…In the present work the r-mode instability has been discussed with reference to the EoS obtained using the density dependent M3Y (DDM3Y) effective nucleonnucleon (NN) interaction [1]. This EoS provides good descriptions for proton, α and cluster radioactivities, elastic and inelastic scattering, symmetric and isospin asymmetric nuclear matter, neutron star masses and radii, their core-crust transition and crustal fraction of moment of inertia [2,3].…”