Stability of the stellar structure and nonequilibrium dynamical characteristics of \((g-T)\) effects in nuclear reactions in stellar cores. (English) Zbl 0792.76029
The nonequilibrium dynamical theory of thermonuclear reaction in the stars is used to analyse the stabilities of \(P-PI\) reactions in the solar core and \(3\alpha\) reactions of helium burning in the core of red giant stars. The constant stability of stars on the main sequence and the helium “flash” instability have been explained from a new point of view. Calculations show that the \((g-T)\) term in the dynamical equation has a damaging effect on the stability of the thermonuclear reaction, but its intensity in the core of red giant stars is \(\sim 10^ 7\) times that in the solar core.
MSC:
| 76E20 | Stability and instability of geophysical and astrophysical flows |
| 76V05 | Reaction effects in flows |
| 85A15 | Galactic and stellar structure |
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