Eur. Phys. J. Plus (2014) 129: 62
https://doi.org/10.1140/epjp/i2014-14062-x

Regular Article

From nuclear reactions to compact stars: A unified approach

¹ Variable Energy Cyclotron Centre, 700 064, Kolkata, India
² Dept. of Physics, Govt. Degree College, 799 285, Kamalpur, Dhalai, Tripura, India
³ Reactor Physics and Nuclear Engineering Section, RRS Division, Bhabha Atomic Research Centre, 400 085, Mumbai, India

^* e-mail: dnb@vecc.gov.in

Received: 21 October 2013
Revised: 14 March 2014
Accepted: 21 March 2014
Published online: 25 April 2014

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 the 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 -equilibrated neutron star matter obtained from this effective interaction for a 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.