Stability of the stellar structure and nonequilibrium dynamical characteristics of \((g-T)\) effects in nuclear reactions in stellar cores (Q1318292)

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.