2025/11/05 by Bisnovatyi-Kogan, G. S., Patraman, E. A.
#FOS: Physical sciences #High Energy Astrophysical Phenomena (astro-ph.HE)
paper · doi:10.48550/arxiv.2511.03419
Stellar models are calculated in the approximation of a uniform density distribution. Variational method was used for determination of the boundary of a stability loss, for stellar masses in the range from 2 up to 105 M\odot. The effects of the general relativity had been taken into account. The equation of state in the temperature and density ranges 109 < T < 1010 K, 105 < ρ< 1010 (g)/(cm3) had been taken from the work of Imshennik and Nadyozhin (1965). The critical parameters for the values of entropy and stellar masses differ from more accurate values, obtained using a more complicated variant of accepted density distribution, not more than 12%.