Neutron star structure and collective excitations of finite nuclei

Abstract

We study relationships between properties of collective excitations in finite nuclei and the phase transition density $n_t$ and pressure $P_t$ at the inner edge separating the liquid core and the solid crust of a neutron star. A theoretical framework that includes the thermodynamic method, relativistic nuclear energy density functionals and the quasiparticle random-phase approximation is employed in a self-consistent calculation of $(n_t,P_t)$ and collective excitations in nuclei. The covariance analysis shows that properties of charge-exchange dipole transitions, isovector giant dipole and quadrupole resonances and pygmy dipole transitions are correlated with the core-crust transition density and pressure. A set of relativistic nuclear energy density functionals, characterized by systematic variation of the density dependence of the symmetry energy of nuclear matter, is used to constrain possible values for $(n_t,P_t)$. By comparing the calculated excitation energies of giant resonances, energy weighted pygmy dipole strength, and dipole polarizability with available data, we obtain the weighted average values: $n_t=0.0955\pm 0.0007$ fm${}^{-3}$ and $P_t=0.59\pm 0.05$ MeV fm${}^{-3}$.

4 pages, 3 figures, paper submitted for publication

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• Decoding rotating neutron stars: Role of the symmetry energy slope
• Two-neutrino double-beta decay matrix elements based on relativistic nuclear energy density functional
• Crust-core interface and bulk neutron star properties
• Correlation between the symmetry energy slope and the deconfinement phase transition
• Constraining neutron star properties through parity-violating electron scattering experiments and relativistic point coupling interactions
• Dipole Polarizability of Finite Nuclei as a Probe of Neutron Stars
• Universal relation between dipole polarizability of finite nuclei and neutron-star compactness