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

Abstract

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 3α 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 ~ 107 times that in the solar core. It may be intimately related to some instability of the stellar structure. The effect on the “flash” instability is especially analysed.