A version of the STARS stellar evolution code has been developed that uses a non-simultaneous solution of the equations of stellar structure and evolution. In all other respects it is identical to the normal, fully simultaneous version. It is therefore possible to test the dependence of the solution on how the equations are solved. Two cases are investigated: a 5- and a 3-M-circle dot star, both of metallicity Z= 0.02. Prior to the asymptotic giant branch, the models are almost identical. However, once thermal pulses start, the two methods of solution yield diverging results with the non-simultaneous technique predicting longer interpulse periods. This is traced to difficulties associated with hydrogen burning caused by the use of a moving mesh. It is shown that, with careful control of the temporal resolution, the results of the simultaneous technique can be recovered.
|Pages (from-to)||1817 - 1822|
|Number of pages||6|
|Journal||Monthly Notices of the Royal Astronomical Society|
|Publication status||Published - 2006|