Dataset referencing 2018KU05

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, 112,116,120,124Sn, 106,116Cd, 122,124,126,128,130Te, 209Bi, 208Pb, 232Th, 238U; calculated neutron skin thicknesses. 36,38,40,42,44,46,48,50,52,54,56,58Ca, 50,52,54,56,58,60,62,64,66,68,70,72,74,76,78,80Ni, 80,82,84,86,88,90,92,94,96,98,100,102,104,106,108,110,112Zr, 102,104,106,108,110,112,114,116,118,120,122,124,126,128,130,132,134,136,138,140Sn, 188,190,192,194,196,198,200,202,204,206,208,210,212,214,216,218,220Pb, 290,292,294,296,298,300,302,304,306,308,310,312,314,316,318,320,322,324,326,328,330,332,334,336,338120; 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

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