Phys.Rev. C 97, 045806 (2018)

B.Kumar, S.K.Patra, B.K.Agrawal

New relativistic effective interaction for finite nuclei, infinite nuclear matter, and neutron stars

NUCLEAR STRUCTURE ¹⁶O, ^40,48Ca, ⁶⁸Ni, ⁹⁰Zr, ^100,132Sn, ²⁰⁸Pb; calculated binding energy per particle, charge radius, and neutron-skin thicknesses. ^40,48Ca, ^58,60,64Ni, ⁵⁹Co, ^54,56,57Fe, ^90,96Zr, ^{112,116,120,124}Sn, ^106,116Cd, ^{122,124,126,128,130}Te, ²⁰⁹Bi, ²⁰⁸Pb, ²³²Th, ²³⁸U; calculated neutron skin thicknesses. ^{36,38,40,42,44,46,48,50,52,54,56,58}Ca, ^{50,52,54,56,58,60,62,64,66,68,70,72,74,76,78,80}Ni, ^{80,82,84,86,88,90,92,94,96,98,100,102,104,106,108,110,112}Zr, ^{102,104,106,108,110,112,114,116,118,120,122,124,126,128,130,132,134,136,138,140}Sn, ^{188,190,192,194,196,198,200,202,204,206,208,210,212,214,216,218,220}Pb, ^{290,292,294,296,298,300,302,304,306,308,310,312,314,316,318,320,322,324,326,328,330,332,334,336,338}120; calculated S(2n). Effective-field-theory relativistic mean-field (E-RMF) model using Institute of Physics Bhubaneswar-I (IOPB-I) interaction. Comparison with results from NL3, FSUGarnet, and G3 models, and with experimental values. Applied IOPB-I to evaluate properties of infinite nuclear matter and neutron stars.

doi: 10.1103/PhysRevC.97.045806