[mesa-users] Resolving core oscillation
Hurst, Travis J
tjh47 at pitt.edu
Thu Feb 11 13:09:39 EST 2016
I have introduced some extra energy transport in the core of a solar mass star. During the RGB phase this extra transport induces thermal pulses and a small convective zone forms at the center. In order to resolve these pulses MESA requires a timestep of order 100 years. This means that the full RGB will require months to run. Are there any timestep controls that might be useful here?
I have also run into an issue when I get to model numbers over 10^6. The photos for restarts are no longer saved correctly and if I do restart, my star will be where it was at 10^5 models instead of at 10^6 though the model number says it is model 10^6.
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