Modelo de una estrella simple con rotación, de la secuencia principal : simulación numérica de una estrella simple con rotación en la secuencia principal.

Abstract

In this work, the behavior of a rotating star on the main sequence was analyzed by solving its stellar structure equations through numerical integration, using the fourth-order Runge-Kutta method. Two specific cases were studied: the poles and the equatorial line of the star. The mass, pressure, and density results were compared in these two cases. Additionally, the effects of different angular velocities were examined, and two distinct formalisms were used: the Newtonian and the post-Newtonian formalisms. It was found that rotation affects the mass and pressure profiles, varying with the star's angular velocity and the physical formalism employed.