Open AccessDoes simultaneous solution matter for stellar evolution codes?
Author(s) -
Stancliffe Richard J.
Publication year - 2006
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2006.10595.x
Subject(s) - physics , metallicity , astrophysics , stellar evolution , asymptotic giant branch , thermal , stars , star (game theory) , star formation , stellar structure , thermodynamics
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 ⊙ 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.