A Method of Computing Stellar Interior Models.
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Abstract
A method of stellar model construction is described which allows easy steps from one model to the next in the course of evolution of a stellar mass. The equations which are solved simultaneously at each time step by using the IBM 704 are the following: the radiation flux equation, an approximate convective flux equation, the electron heat conduction equation, the equation of momentum conservation, and the conservation of energy equation. The calculation is done in a Lagrangian coordinate system making the conservation of mass equation very simple. Standard energy generation expressions are used. We have calculated the equations of state and opacities as needed. These data include, among other details, the effects of radiation pressure and energy, and those of electron degeneracy. Solution of these simultaneous equations at each time step allows one to watch the one-space-dimensional relaxation of stellar mass to its equilibrium in all the nonlinear nonadiabatic detail. Some results for one solar mass are given.
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