The isovector density-dependence of the M3Y nucleon-nucleon interactions and related soft and hard equations of state

Mass–radius relation of neutron stars and massive pulsars with realistic equation of state

“…It was shown that the incompressibility at maximum density of nuclear β-stable NM in NS determines the behavior of binary neutron star mergers near prompt collapse and the related influence of the mass ratio [94]. Moreover, the more specific EOSs of CDM3Y-Paris (K 0 = 240-250 MeV) and Reid (K 0 = 230-240 MeV), which are involved in the present anticipated range of EOSs, were reported in [32,49] to perform simultaneous consistency assessment with experimental constraints and precise calculations on symmetric and asymmetric NM and pure neutron matter energy and pressure. The above mentioned endorsed EOSs from K 0 = 230 to 270 MeV of Paris (Reid) NN interaction are characterized with symmetry energy coefficient S = 29.100 ± 0.004 MeV (30.979 MeV) and corresponding density-slope of symmetry energy is L = 48.205 ± 0.005 MeV (50.805 ± 0.019 MeV).…”

“…In the present work, the EOS of the npem matter of the outer core of NS will be extended to describe its inner core as well [9,22,63]. The energy per nucleon (E A ) in equation (1) can be obtained based on the CDM3Y density dependent form [64] of the M3Y-Paris [65] and M3Y-Reid [66] NN interactions by [32,49]…”

“…a b g ) [49] were obtained for different CDM3Y-K 0 parameterizations, which describe a broad range of soft and stiff EOSs characterized by saturation incompressibility values   K 150 MeV 300 MeV.…”

“…While the isoscalar density dependence parameters were obtained through explicit calculations [49], the isovector parameters have been obtained by fitting the calculated isovector neutron potential with the Brueckner-Hartree-Fock results provided by Jeukenne, Lejeune, and Mahaux [68,69]. In the present work, we have determined the density dependence parameters for the stiffer CDM3Y-330 EOS of Paris (Reid) NN interactions to read c 0 = 2.4624(3.7679), α 0 = −0.5273 (−0.7133), β 0 = 2.4741 fm 3 (2.1758 fm 3 ), γ 0 = 1.7431 fm 3 (1.5634 fm 3 ), c 1 = 0.2199 (0.161), α 1 = 7.8 (8.789), β 1 = 9.2999 fm 3 (9.8532 fm 3 ), and γ 1 = −6.9579 fm 3 (−7.811 fm 3 ).…”

“…These interactions are used frequently, with a high degree of confidence, to study nuclear structure [38,39], reactions [40][41][42][43][44], and decays [45][46][47]. Soft and stiff EOSs based on the two considered interactions, with incompressibility coefficient values ranging between 150 and 300 MeV, have been used in non-relativistic Hartree-Fock framework to investigate the symmetry [48,49] and saturation [50] properties of cold [32,51] and hot [28,52] NM, as well as β-stable neutron star matter [22,30,53] investigations. The mass-radius relation of neutron stars and massive pulsars and the different particle contributions to their core matter will be investigated in terms of the considered EOSs based on the realistic Michigan-three-Yukawa (M3Y)-Reid and M3Y-Paris NN interactions.…”