Energy Levels Calculations of 20Ne and 21Ne Isotopes
American Journal of Modern Physics
Volume 4, Issue 3-1, May 2015, Pages: 36-39
Received: Mar. 2, 2015; Accepted: Mar. 4, 2015; Published: Mar. 10, 2015
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Authors
Saeed Mohammadi, Department of Physics, Payame Noor University, PO BOX 19395-3697 Tehran, Iran
Maryam Mounesi, Department of Physics, Payame Noor University, PO BOX 19395-3697 Tehran, Iran
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Abstract
In this article by using OXBASH shell model code the energy levels of Neon isotopes 20Ne and 21Ne are calculated. This code which is based on one of the most applicable nuclear models, deals with evaluating energy levels. Applying the program for each isotope using the defined codes, introduces several files which each file contains a set of data. Meanwhile, the ground state of excitation energy evaluated by OXBASH code together with energy levels and also probable places for nucleons’ placements in each energy level. Programs will be reliable only when results meet experimental procedures. A compilation of SD-shell energy levels calculated with the USD Hamiltonian and has been published around 1988. A comparison had been made between our results and the available experimental data to test theoretical shell model description of nuclear structure in Neon isotopes. The calculated energy spectrum is in good agreement with the available experimental data.
Keywords
Neon Isotopes, OXBASH Code, Shell Model Structure, USD Interaction
To cite this article
Saeed Mohammadi, Maryam Mounesi, Energy Levels Calculations of 20Ne and 21Ne Isotopes, American Journal of Modern Physics. Special Issue: Many Particle Simulations. Vol. 4, No. 3-1, 2015, pp. 36-39. doi: 10.11648/j.ajmp.s.2015040301.18
References
[1]
Nuclear Physics Graduate Course: Nuclear Structure Notes, Oxford, (1980)
[2]
Effective interactions and the nuclear shell-model, D.J. Dean,T. Engeland M. Hjorth-Jensen, M.P. Kartamyshev, E. Osnes, Progress in Particle and Nuclear Physics 53 419–500(2004)
[3]
N. A. Smirnova, Shell structure evolution and effective in-medium NN interaction, Chemin du Solarium, BP 120, 33175 Gradignan, France
[4]
Oxbash for Windows, B. A. Brown, A. Etchegoyen, N. S. Godwin, W. D.M. Rae, W.A. Richter, W.E. Ormand, E.K. Warburton, J.S. Winfield, L. Zhao and C.H. Zimmerman, MSU_NSCL report number 1289.
[5]
W. A. Richter, M. G. van der Merwe, R. E. Julies, B. A. Brown, Nucl. Phys. A 523,325, (1991)
[6]
R. E. Julies, PhD. thesis, University of Stelenbosch, (1990).
[7]
M. G. van der Merwe, PhD. thesis, University of Stelenbosch (1992).
[8]
B. H. Wildenthal, Prog. Part. Nucl.Phys. 11, 5 (1984).
[9]
B. A. Brown and B. H. Wildenthal, Ann. Rev. of Nucl. Part. Sci. 38, 29 (1988).
[10]
http://www.nscl.msu.edu/~brown/
[11]
B.A. Brown, W.A. Richter, New “USD”Hamiltonians for the sd shell, Physical Review C, 74 (2006)
[12]
http://www.nscl.msu.edu/~brown/resources/SDE.HTM#a34t2
[13]
B.H. Wildenthal, Prog. Part. Nucl. Phys. 11, 5 (1984), and references therein
[14]
M. Homma, B. A. Brown, T. Mizusaki and T. Otsuka, Nucl. Phys.A 704, 134c (2002)
[15]
B. A. Brown and W. A. Richter, Phys. Rev. C 74, 034315, (2006).
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