This stellar evolution package is meant as a learning tool. There are many things that can be improved, e.g. opacity, equation of state, nuclear burning, etc. and the routines are not always optimized for performance or accuracy. On a unix machine the following should calculate the evolution of a 1 solar mass star from the "birthline" (standard composition, equilibrium deuterium burning) to well into the red giant phase at the beginning of core helium burning... $ make all $ polytr < polytr1.inp $ stellar < pmsstar1.start > pmsstar1.lst $ stellar < pmsstar1.inp >> pmsstar1.lst The .inp file is set up to run 500 models at a time. The evolution of a 3 solar mass star from the birthline well into helium shell burning is calculated with $ polytr < polytr3.inp $ stellar < pmsstar3.start > pmsstar3.lst $ stellar < pmsstar3.inp >> pmsstar3.lst The .inp file is set up to continue running until the program reaches an error exit.
lruhlen/Original_Peter_Code
Peter Bodenheimer's original Fortran code for modeling the interior structure of stars.
Fortran