Simple Effective Interaction: From Finite Nucleus to Neutron Stars

Abstract: The background of the formulation of the Simple Effective Interaction (SEI) is discussed. The systematics of its parameter fixation protocol is outlined that could account for the divergent trends on the density and momentum dependence of the isovector part of the nucleonic mean field predictions by different model calculations. 

The r-mode oscillation as a possible mechanism for the spin-down feature of newborn neutron stars is discussed. The ability of the bulk viscosity due to direct Urca processes in dissipating the large oscillations produced in the merger remnant in the event of two neutron star merger is examined where the equation of state of hot neutron star matter of neutron-proton-electron-muon composition is built upon it’s zero-temperature predictions.  

The predictions of SEI in different areas of finite nuclei properties is discussed. The correlation between the finite nuclei properties and the constraints resulting from neutron star phenomenology is examined using the charge radii differences in mirror nuclei pairs as observable.