Abstract
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 \({{10}^{5}}{\kern 1pt} {{M}_{ \odot }}\) . The effects of the general relativity had been taken into account. The equation of state in the temperature and density ranges \({{10}^{9}} < T{{ < 10}^{{10}}}\) K, \({{10}^{5}} < \rho {{ < 10}^{{10}}}\) 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%.
