[Mesa-users] Stellar rotation

[Jared Goldberg]

MESA is able to handle many radiative and convective zones, as it locally
checks whether the zone should be radiative or convective at every zone in
the model.

To do this, MESA calculates the Schwartzschild or Ledoux criterion (see
documentation
<https://docs.mesastar.org/en/latest/reference/controls.html#use-ledoux-criterion>
for turning this on) for convective instability in each shell in the model.
This is a local condition, so MESA may calculate many radiative and
convective layers, and switches energy transport between them. Typically
MESA implements convection via Mixing Length Theory (See e.g. review by Joyce
& Tayar <https://ui.adsabs.harvard.edu/abs/2023Galax..11...75J/abstract>),
with the added capability of doing time-dependent convection (described in
MESA VI <https://ui.adsabs.harvard.edu/abs/2023ApJS..265...15J/abstract>).

For an example of a star with many layers (convective cores and shells and
radiative zones too and a convective envelope), see e.g. the
$MESA_DIR/star/test_suite/12M_pre_ms_to_core_collapse/ case in the
test_suite, which takes a star to core-collapse which develops many layers
of radiation and convection in between.

The rest will depend on the science case you have in mind -- what kind of
star do you have in mind? What are you trying to learn about it?

~Jared

On Tue, Sep 17, 2024 at 12:52 PM Viviana Beatríz Bolzicco via Mesa-users <
mesa-users at lists.mesastar.org> wrote:

> Dear all
>
> I'm just beginning to use MESA and I'm reading Bill Paxton et al (2013)'s
> Modules for experiments in stellar astrophysics (MESA): Planets,
> Oscillations, Rotation, and Massive stars.
> I'm interested to know how you resolve the problem of a star with more
> than one radiative zone.
>
> Regards
>
>  Viviana B. Bolzicco
> _______________________________________________
> mesa-users at lists.mesastar.org
> https://lists.mesastar.org/mailman/listinfo/mesa-users
>
>
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