Mathematical model for the 0:85 billion year sun

Abstract

An algorithm for constructing evolutionary tracks for a star with a mass equal to one solar mass is given. The model presented can be applied to the stars belonging to the inferior main sequence, which have the proton-proton reaction as an energy source and present a radiative core and a convective shell. This paper presents an original way of resolving the system of equations corresponding to the radiative nucleus by using Taylor's series in close vicinity to the center of the Sun. It also presents the numerical integration and the results for a 0:85 billion year solar model.