Exciton Model Calculations up to 200 MeV: The Optical Model Points the Way

2005 ◽  
Author(s):  
M. C. Duijvestijn
2015 ◽  
Vol 24 (01) ◽  
pp. 1550006 ◽  
Author(s):  
Yuan Tian ◽  
Dan-Yang Pang ◽  
Zhong-Yu Ma

Based on the Perey–Buck nonlocal optical model potential, F. Perey and B. Buck, Nucl. Phys. 32 (1962) 353, we obtain a new set of nonlocal optical model potential (NLOMP) parameters for proton and neutron scattering off nuclei. The experimental angular distributions of nucleon scattering off nuclei ranging from 27 Al to 208 Pb with incident energies around 10 MeV to 30 MeV are adopted in the fitting procedures. This NLOMP is energy independent. The chi-squares χ2 obtained in the fittings are comparable to those from the KD03 phenomenological local optical model potentials (OMP) A. Koning and J. Delaroche, Nucl. Phys. A 713 (2003) 231. Good agreement is found in comparisons between optical model calculations using this NLOMP and KD03 in their reproduction to the experimental angular distributions of elastic scattering cross-sections and analyzing powers.


1996 ◽  
Vol 22 (3) ◽  
pp. 387-396 ◽  
Author(s):  
R R Dubey ◽  
G S Khandelwal ◽  
F A Cucinotta ◽  
J W Wilson

1992 ◽  
Vol 01 (04) ◽  
pp. 823-831 ◽  
Author(s):  
B. P. SINGH ◽  
M. G. V. SANKARACHARYULU ◽  
M. A. ANSARI ◽  
R. PRASAD ◽  
H. D. BHARDWAJ

Excitation functions for 209 Bi (α, 3n), 209 Bi (α, 4n) and 209 Bi (α, 5n) reactions have been measured in the energy range threshold to ≈50 MeV using stacked foil technique. Excitation functions have also been theoretically calculated and as expected, inclusion of pre-equilibrium contribution based on exciton model calculations along with compound nucleus calculations using Hauser–Feshbach formalism reproduces well the measured excitation functions. Interesting trend in the ratio of pre-equilibrium to equilibrium component with projectile energy has been observed.


1995 ◽  
Vol 48 (1) ◽  
pp. 125
Author(s):  
A.J Morton ◽  
DG Sargood

Nuclear reaction cross sections derived from statistical-model calculations have been used in the calculation of thermonuclear reaction rates for 36 nuclei at temperatures that are representative of the interiors of evolving stars and supernovae as nucleosynthesis approaches the production of nuclei with N = 28. The statistical-model calculations used optical-model parameters in the particle channels which had been selected to give the best overall agreement between theoretical and experimental cross sections for reactions on stable target nuclei in the mass and energy ranges of importance for the stellar conditions of interest. The optical-model parameters used, and the stellar reaction rates obtained, are tabulated. Comparisons are made between these stellar rates and those from other statistical-model calculations in the literature.


1994 ◽  
Vol 49 (3) ◽  
pp. 1609-1620 ◽  
Author(s):  
Anders Ingemarsson ◽  
Agris Auce ◽  
Roger Johansson

2017 ◽  
Vol 146 ◽  
pp. 12013 ◽  
Author(s):  
José Manuel Quesada ◽  
Dmitry Martyanov ◽  
Efrem Soukhovitskiĩ ◽  
Roberto Capote ◽  
Satoshi Chiba

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