A Numerical Solar Model

A basic model of stellar structure is presented here. The sun is initially modeled using four fundamental equations of stellar structure. Since these equations are not analytically solvable, they were solved numerically using the Runge-Kutta fourth order approximation. Despite several firstorder approximations that were made, resulting values for density, mass, luminosity, and temperature were correct to relative error on the order of 10^-7. The inclusion of variable chemical composition increased the accuracy of the model further still. The internal error of the numerical analysis was also on the order of 10^-7, which showed the dependability of our rudimentary models. Throughout, the mechanisms of opacity and energy generation in the stellar model are addressed.