.. _ZAMS_to_core_collapse_80:

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ZAMS_to_core_collapse_80
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.. tags:: star, very-massive-star, pre-main-sequence, full-evolution, core-collapse, mass-loss, wolf-rayet, carbon-burning, silicon-burning

This test suite evolves a solar metalicity 80 |MSun| model from the pre-ms to core collapse with mass loss.
A strong mass loss rate is adopted to make a Wolf-rayet star that is ~37 Msun, below the threshold for pair instability.
For bit for bit convergence, we recommended to run by using the ./run_all script instead of restarting from models,
see https://github.com/MESAHub/mesa/issues/610.

This test_suite has been tested up to 80 solar masses, up to solar metallicity, with mass loss, and produces reasonable HR-tracks.
Note that for higher masses at solar metallicity, some combination of Pextra_factor, mass-loss, and/or superadiabatic convection reduction (e.g. mlt++)
might be necessary to stabilize the surface and avoid numerical issues.

For production science we recommend adopting tighter mesh and timestep controls, such as those suggested in the comments of inlist_common.

Physical checks
===============

None

Inlists
=======

This test case has seven parts.

* Part 1 (``inlist_make_late_pre_zams``) creates a 80 |Msun|, Z=1.42*10^-2 metallicity, pre-main sequence model and evolves it for 100 years.

* Part 2 (``inlist_to_zams``) evolves the model to the zero age main sequence.

* Part 3 (``inlist_to_end_core_he_burn``) takes the model to core helium depletion.

* Part 4 (``inlist_remove_envelope``) removes the remaining hydrogen envelope. (optional)

* Part 5 (``inlist_to_end_core_c_burn``) takes the model to core carbon depletion.

* Part 6 (``inlist_to_lgTmax``) evolves the model until the core temperature reaches log T =9.60 (approximately silicon-shell burning)

* Part 7 (``inlist_to_cc``) evolves until core collapse.


Last-Updated: 18Dec2023 by EbF