Theory of Finite Systems and Applications to Atomic Nuclei

Physics Today ◽  
1969 ◽  
Vol 22 (6) ◽  
pp. 85-87
Author(s):  
A. B. Migdal ◽  
John L. Gammel
Keyword(s):  
2020 ◽  
Vol 2 (4) ◽  
pp. 529-541
Author(s):  
Angelo Plastino ◽  
Diana Monteoliva ◽  
Angel R. Plastino

We investigate finite systems of N paired fermions, common in atomic nuclei, for example. These systems exhibit quantum mechanical features akin to those of superconductors. We discover, however, some specific N dependent effects that can not be attained in the thermodynamics limit of ordinary superconductivity. In particular, an important fact is uncovered: there is a strong correlation between the temperature T and the number of fermions N. A certain temperature increase ΔT produces, in thermal quantifiers (such as the entropy), quite different effects if N=4 or N=25. In fact, whether a given temperature value should be regarded as high or low can not be ascertained independent of the N value.


2020 ◽  
Author(s):  
Rostislav V. Jolos ◽  
Elena A. Kolganova

1963 ◽  
Vol 81 (10) ◽  
pp. 271-334 ◽  
Author(s):  
L.A. Borisoglebskii
Keyword(s):  

Author(s):  
Rostislav V. Jolos ◽  
Elena A. Kolganova

Author(s):  
Р. М. Плекан ◽  
В. Ю. Пойда ◽  
І. В. Хіміч

Author(s):  
E. L. Wolf

Protons in the Sun’s core are a dense plasma allowing fusion events where two protons initially join to produce a deuteron. Eventually this leads to alpha particles, the mass-four nucleus of helium, releasing kinetic energy. Schrodinger’s equation allows particles to penetrate classically forbidden Coulomb barriers with small but important probabilities. The approximation known as Wentzel–Kramers–Brillouin (WKB) is used by Gamow to predict the rate of proton–proton fusion in the Sun, shown to be in agreement with measurements. A simplified formula is given for the power density due to fusion in the plasma constituting the Sun’s core. The properties of atomic nuclei are briefly summarized.


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