Stability of the Shells of the Heaviest Atomic Nuclei in the Semi-relativistic Model

2020 ◽  
pp. 211-220
Keyword(s):  
Relativistic Model ◽  
Atomic Nuclei

Phase transitions in atomic nuclei

2020 ◽  
Author(s):  
Rostislav V. Jolos ◽  
Elena A. Kolganova
Keyword(s):  
Phase Transitions ◽  
Atomic Nuclei

Monopole transitions of atomic nuclei

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

Phase transitions in atomic nuclei

2020 ◽  
Author(s):  
Rostislav V. Jolos ◽  
Elena A. Kolganova
Keyword(s):  
Phase Transitions ◽  
Atomic Nuclei

Theoretical description of nucleons correlations of even-even atomic nuclei

2003 ◽  
Vol 14 (0) ◽  
pp. 40-45
Author(s):  
Р. М. Плекан ◽  
В. Ю. Пойда ◽  
І. В. Хіміч
Keyword(s):  
Theoretical Description ◽  
Atomic Nuclei

Fusion in the Sun

2018 ◽  
Author(s):  
E. L. Wolf
Keyword(s):  
Kinetic Energy ◽  
Power Density ◽  
Dense Plasma ◽  
Alpha Particles ◽  
The Sun ◽  
Proton Proton ◽  
Atomic Nuclei ◽  
Proton Fusion ◽  
Schrödinger's Equation ◽  
Simplified Formula

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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