[Mesa-users] Evolving 2–3 M☉ models from TAMS to Red Clump for GYRE

[Meridith Joyce]

Hi Bruno,

Using GYRE on-the-fly, as discussed here (and see related Zenodo / Github
links and citations) might be a good place to start:
https://ui.adsabs.harvard.edu/abs/2024ApJ...971..186J/abstract
The code to do this is public.

There are evolutionary phase-based stopping conditions defined in MESA, of
the form "stop_at_TACHeB = true" or similar. You can find a list of these
and their physical definitions in mesa/star/private/star_utils.f90 (search
"phase_of_evolution").

Cheers,

On Thu, Jun 12, 2025 at 4:27 PM Bruno Lustosa via Mesa-users <
mesa-users at lists.mesastar.org> wrote:

> Hello everyone,
>
> I’m currently using the `1M_pre_ms_to_wd` test case from the
> `mesa-24.08.1` release.
>
> My goal is to evolve a grid of stars with masses between 2.0 and 3.0 M☉,
> with varying initial_z, but I’m only interested in the evolutionary phase
> from the Terminal Age Main Sequence (TAMS) to the Red Clump.
>
> I would appreciate suggestions on how to:
>
> 1. Stop the evolution at TAMS and resume from that point (or start
> directly near the TAMS),
> 2. Define a suitable stopping condition at the clump (e.g., core
> He-burning onset or a threshold He-burning luminosity),
> 3. Generate output suitable for use with GYRE, including proper
> profile_columns.list and high-resolution models.
>
> If anyone has recommendations on inlist setup, stopping flags, or
> resolution adjustments for this evolutionary stage, I’d be very grateful.
>
> Best regards,
> Bruno
> _______________________________________________
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>

-- 

Assistant Professor Meridith Joyce, PhD
Department of Physics and Astronomy
& School of Computing
College of Engineering and Physical Sciences
University of Wyoming
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