Empirical formula on (n, 3 He) reaction cross sections at 14.6 MeV neutrons

2015 ◽  
Vol 105 ◽  
pp. 15-19 ◽  
Author(s):  
Mustafa Yiğit
Keyword(s):  
Cross Sections ◽  
Empirical Formula ◽  
Reaction Cross ◽  
Reaction Cross Sections

New Evaluated Semi-Empirical Formula Using Optical Model for 14–15 MeV (n, t) Reaction Cross Sections

2009 ◽  
Vol 28 (4) ◽  
pp. 377-384 ◽  
Author(s):  
E. Tel ◽  
C. Durgu ◽  
A. Aydın ◽  
M. H. Bölükdemir ◽  
A. Kaplan ◽  
...  
Keyword(s):  
Cross Sections ◽  
Empirical Formula ◽  
Optical Model ◽  
Reaction Cross ◽  
Semi Empirical ◽  
Reaction Cross Sections

New empirical formula for calculating (n,p) reaction cross-sections at 14.5MeV neutrons

2020 ◽  
Vol 29 (08) ◽  
pp. 2050052
Author(s):  
Dashty T. Akrawy ◽  
Ali H. Ahmed ◽  
E. Tel ◽  
A. Aydin ◽  
L. Sihver
Keyword(s):  
Cross Section ◽  
Cross Sections ◽  
Empirical Formula ◽  
Nuclear Data ◽  
Reaction Cross ◽  
Section Data ◽  
Nuclear Data Library ◽  
Number Formula ◽  
New Formula ◽  
Reaction Cross Sections

An empirical formula to calculate the ([Formula: see text], [Formula: see text] reaction cross-sections for 14.5[Formula: see text]MeV neutrons for 183 target nuclei in the range [Formula: see text] is presented. Evaluated cross-section data from TENDL nuclear data library were used to test and benchmark the formula. In this new formula, the nonelastic cross-section term is replaced by the atomic number [Formula: see text], while the asymmetry parameter-dependent exponential term has been retained. The calculated results are presented in comparison with the seven previously published formulae. We show that the new formula is significantly in better agreement with the measured values compared to previously published formulae.

Systematics of (n,p) reaction cross-sections for light element target nuclei at 14.5MeV neutrons

2018 ◽  
Vol 27 (10) ◽  
pp. 1850079 ◽  
Author(s):  
Ali Hassan Ahmed
Keyword(s):  
Cross Sections ◽  
Empirical Formula ◽  
Light Element ◽  
Nuclear Data ◽  
Reaction Cross ◽  
Incident Neutron ◽  
Number Range ◽  
Proton Separation Energy ◽  
Nuclear Data Library ◽  
Reaction Cross Sections

The systematics of neutron-induced reactions at 14.5[Formula: see text]MeV are of great importance to describe the excitation of nuclei for the [Formula: see text] reactions. In this study, a new empirical formula is obtained by introducing the proton separation energy to the principal empirical formula for estimating the [Formula: see text] reaction cross-sections for 77 nuclei in the light element mass number range [Formula: see text] at the incident neutron energy of 14.5[Formula: see text]MeV. The calculated results are compared with the evaluated data declared by the TENDL nuclear data library. The predictions of our formula reveal better agreement with the experimental data than the results obtained from the previous suggested formulae.

Formation of α clusters in dilute neutron-rich matter

Science ◽  
2021 ◽  
Vol 371 (6526) ◽  
pp. 260-264 ◽  
Author(s):  
Junki Tanaka ◽  
Zaihong Yang ◽  
Stefan Typel ◽  
Satoshi Adachi ◽  
Shiwei Bai ◽  
...  
Keyword(s):  
Cross Sections ◽  
Cluster Formation ◽  
Reaction Cross ◽  
Skin Thickness ◽  
Neutron Skin ◽  
Heavy Nuclei ◽  
Α Decay ◽  
Neutron Skin Thickness ◽  
Reaction Cross Sections ◽  
Α Particles

The surface of neutron-rich heavy nuclei, with a neutron skin created by excess neutrons, provides an important terrestrial model system to study dilute neutron-rich matter. By using quasi-free α cluster–knockout reactions, we obtained direct experimental evidence for the formation of α clusters at the surface of neutron-rich tin isotopes. The observed monotonous decrease of the reaction cross sections with increasing mass number, in excellent agreement with the theoretical prediction, implies a tight interplay between α-cluster formation and the neutron skin. This result, in turn, calls for a revision of the correlation between the neutron-skin thickness and the density dependence of the symmetry energy, which is essential for understanding neutron stars. Our result also provides a natural explanation for the origin of α particles in α decay.

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