Separation energies of light nuclei with atomic number from 1 to 20

P. Mandal, R. L. Nayak, T. Sahoo, Anjana Acharya


The 1n and 1p halo nuclei from atomic number 1 to 20 are discussed here to calculate the variation of separation energy with mass defect and binding energy. Semi-empirical mass formula and shell model are the methods applied here. The appearances of p- and r-branches satisfying the selection rules for different isotopes of nuclides are discussed.


shell model, halo nuclei, separation energy, r- and p- processes

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Takao Tati, “Separation energies and nuclear structures in light nucleiâ€, Progress of Theoretical Physics, 14, 2 (1955)

A. Athanassopoulos, E. Mavrommatics K. A. Gernoth W. Clark, “One and two proton separation energies from mass systematics using neural networksâ€, Nuclear Physics A, 743, 222 (2004)

K. Vogt, T. Hartmann, A. Zilges, “Simple parametrization of single and two nucleon separation energy in terms of the N/Zâ€, Physics Letters B, 517, 255 (2001)

M. Arnould, K. Takahashi, “Nuclear Astrophysicsâ€, Reports on Progress in Physics, 62, 395 (1999)

M. T. Yamashita, R. S. Marques de Carvalho, T. Frederico, Lauro Tomio, “Constraints on 2n separation energy in Borromean 22C nucleusâ€, Physics Letter B, 697, 90 (2011)


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