Nuclear Science References (NSR)

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NSR database version of May 1, 2024.

Search: Author = M.Q.Lin

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2022LI07 Phys.Rev. C 105, L021305 (2022)

M.Q.Lin, C.Ma, Y.M.Zhao

Evolution of collectivity and neutron-proton interactions

NUCLEAR STRUCTURE Z=28-82, N=50-82; Z=50-82, N=82-126; analyzed energies of first 2+, 4+ states, integrated neutron-proton interactions V_np; deduced correlation between the evolution of collective motions and V_np.

doi: 10.1103/PhysRevC.105.L021305
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2022SH45 Phys.Rev. C 106, L061304 (2022)

R.Shou, X.Yin, C.Ma, M.Q.Lin, Y.M.Zhao

Simple corrections in theoretical models of atomic masses and nuclear charge radii

ATOMIC MASSES Z=29-110; N=20-160; A=49-270; analyzed systematic root mean square deviations of mass excesses, S(n), and S(p) between their experimental values from AME2020, and theoretical values from Hartree-Fock-Bogoliubov (HFB31), relativistic mean field (RMF), Duflo-Zuker (DZ), and Weizsaker-Skyrme (WS4+RBF) models using strong and specific correlations of these deviations, and deducing Pearson correlation coefficients for 3258 neutron- and proton-rich nuclei listed in the Supplemental Material of the paper.

NUCLEAR STRUCTURE Z=29-59; Z=61-64; Z=66; Z=68-76; Z=78, 79; Z=81-84; Z=86-88; Z=90, 92, 95, 96; analyzed systematic root mean square deviations of charge radii between their experimental values taken from 2021Li25 (Atomic Data and Nuclear Data Tables 140, 101440 (2021)), and theoretical values from Hartree-Fock-Bogoliubov (HFB31), relativistic mean field (RMF), relativistic continuum Hartree-Bogoliubov (RCHB), and Weizsaker-Skyrme (WS*) models using strong and specific correlations of these deviations, and deducing Pearson correlation coefficients for neutron- and proton-rich nuclei listed in the Supplemental Material of the paper.

doi: 10.1103/PhysRevC.106.L061304
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2022ZO01 Phys.Rev. C 105, 034321 (2022)

Y.Y.Zong, C.Ma, M.Q.Lin, Y.M.Zhao

Mass relations of mirror nuclei for both bound and unbound systems

ATOMIC MASSES ³He, ^6,7Be, ^8,9B, ^8,9,10,11C, ^11,12,13N, ^{11,12,13,14,15}O, ^14,15,16,17F, ^{14,15,16,17,18,19}Ne, ^{17,18,19,20,21}Na, ^{17,18,19,20,21,22,23}Mg, ^{20,21,22,23,24,25}Al, ^{21,22,23,24,25,26,27}Si, ^{23,24,25,26,27,28,29}P, ^{24,25,26,27,28,29,30,31}S, ^{27,28,29,30,31,32,33}Cl, ^{28,29,30,31,32,33,34,35}Ar, ^{31,32,33,34,35,36,37}K, ^{32,33,34,35,36,37,38,39}Ca, ^{35,36,37,38,39,40,41}Sc, ^{36,37,38,39,40,41,42,43}Ti, ^{39,40,41,42,43,44,45}V, ^{40,41,42,43,44,45,46,47}Cr, ^{43,44,45,46,47,48,49}Mn, ^{44,45,46,47,48,49,50,51}Fe, ^{47,48,49,50,51,52,53}Co, ^{48,49,50,51,52,53,54,55}Ni, ^{50,51,52,53,54,55,56,57}Cu, ^{52,53,54,55,56,57,58,59}Zn, ^{54,55,56,57,58,59,60,61}Ga, ^{56,57,58,59,60,61,62,63}Ge, ^{60,61,62,63,64,65}As, ^{62,63,64,65,66,67}Se, ^{65,66,67,68,69}Br, ^{67,68,69,70,71}Kr, ^70,71,72,73Rb, ^{71,72,73,74,75}Sr, ^74,75,76,77Y, ^{75,76,77,78,79}Zr, ^78,79,80,81Nb, ^{79,80,81,82,83}Mo, ^82,83,84,85Tc, ^84,85,86,87Ru, ^86,87,88,89Rh, ^88,89,90,91Pd, ^90,91,92,93Ag, ^92,93,94,95Cd, ^94,95,96,97In, ^96,97,98,99Sn; calculated S(p), S(2p), mass excesses for proton-rich systems, both inside and outside the proton drip line, in terms of mass relations for mirror nuclei, based on Weizsacker mass formula. Comparison with available evaluated experimental data from AME2020, and deduced root-mean-square deviations (RMSD).

doi: 10.1103/PhysRevC.105.034321
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2019YU03 Phys.Rev. C 100, 014314 (2019)

H.C.Yu, M.Q.Lin, M.Bao, Y.M.Zhao, A.Arima

Empirical formulas for nuclear separation energies

NUCLEAR STRUCTURE ^{70,71,72,73,74,75,76,77,78,79,80,81,82,83,84,85,86,87,88,89,90,91,92,93,94,95,96,97,98,99,100}Zn, ^{112,113,114,115,116,117,118,119,120,121,122,123,124,125,126,127,128,129,130,131,132,133,134,135,136,137}Mo, ^{151,152,153,154,155,156,157,158,159,160,161,162,163,164,165,166,167,168,169,170,171,172,173,174,175,176,177,178,179,180,181,182,183,184,185,186}Ba, ^{204,205,206,207,208,209,210,211,212,213,214,215,216,217,218,219,220,221,222,223,224,225,226,227,228,229,230,231,232,233,234,235,236,237,238,239}W; calculated S(n) and S(p) using empirical formulas. Comparison with AME-2016 evaluation, and with other theoretical model predictions.

doi: 10.1103/PhysRevC.100.014314
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2019ZO02 Phys.Rev. C 100, 054315 (2019)

Y.Y.Zong, M.Q.Lin, M.Bao, Y.M.Zhao, A.Arima

Mass relations of corresponding mirror nuclei

ATOMIC MASSES ²¹Na, ^22,23Mg, ^23,24,25Al, ^24,25,26,27Si, ^26,27,28,29P, ^28,29,30,31S, ^30,31,32,33Cl, ^32,33,34,35Ar, ^34,35,36,37K, ^36,37,38,39Ca, ^38,39,40,41Sc, ^40,41,42,43Ti, ^42,43,44,45V, ^44,45,46,47Cr, ^46,47,48,49Mn, ^48,49,50,51Fe, ^50,51,52,53Co, ^52,53,54,55Ni, ^54,55,56,57Cu, ^56,57,58,59Zn, ^58,59,60,61Ga, ^60,61,62,63Ge, ^62,63,64,65As, ^64,65,66,67Se, ^66,67,68,69Br, ^68,69,70,71Kr, ^70,71,72,73Rb, ^72,73,74,75Sr, ^74,75,76,77Y, ^76,77,78,79Zr, ^79,80Nb, ^81,83Mo, ^83,85Tc, ^85,86,87Ru, ^87,88Rh, ⁸⁹Pd; calculated mass excesses, S(n), S(p) using mass relations for corresponding mirror nuclei, and compared with AME2016 values; deduced regularities related to neutron-proton interactions, and to separation energies for mirror nuclei.

doi: 10.1103/PhysRevC.100.054315
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