2020/09/30 by Ishfaq Ahmad Rather, Anisul Ain Usmani, Suresh Kumar Patra · 1 citation
Physics and Astronomy · #nucl-th #astro-ph.HE
paper · pdf · doi:10.1016/j.nuclphysa.2021.122189
published as Nuclear Physics A 1010 (2021) 122189 · 27 pages, 14 figures, 2 tables
arxiv created 2021/03/18 · arxiv updated 2021/03/19
The neutron star maximum mass and the radius are investigated within the framework of the relativistic mean-field (RMF) model. The variation in the radius at the canonical mass, R1.4, using different inner crust equation of state (EoS) with different symmetry energy slope parameter is studied. It is found that although the NS maximum mass and the corresponding radius do not vary much with different inner crust EoSs, the radius and the tidal deformability at 1.4M\odot vary with the different choice of crust EoS and variation of about 1-2 km is seen in the radius at the canonical mass. For non-unified EoSs, the crust with a low symmetry energy slope parameter produces a low NS radius at the canonical mass. The properties of maximally rotating neutron stars are also studied. The variation in the radius of rotating star at the canonical mass 1.4M\odot is also seen with the slope parameter. Similar to the static neutron star, the radius at 1.4M\odot of rotating neutron star is affected by slope parameter of the inner crust. Other important quantities like moment of inertia, frequency, rotational kinetic energy to gravitational energy ratio are also calculated. The variation in these quantities with the crust slope parameter is found to be more proportional to the mass and the radius of NS.