[Mesa-users] Evolution of pop III stars up to core-collapse with rotation

[Ramandeep Gill]

Hello MESA experts,

I'm trying to obtain the pre-core-collapse structure of massive pop
III stars to study the launching and propagation of GRB jets in these
stars. In the end, I'm looking to obtain the density and angular
momentum radial profile of the star.

To this end, I've tried a few inlists, starting from the bare minimum
one used for introductory MESA tutorials as well as more advanced ones
from the MESA test suite and any that I could find online. The end
result in all is that after core He depletion, the code crashes most
of the time or, if I manage to somehow stabilize it, settles onto a
spurious solution with a lot of wild oscillations.

I attach an HR diagram from one of the runs for which I used the
inlist from the 'make_pre_ccsn_IIp' test suite example. The evolution
up to H core depletion, He core depletion, and that beyond He core
depletion is color coded. You can see that the last part of the
evolution results in spurious oscillations, after which the code many
times crashes or keeps chugging along at smaller and smaller time
steps.

To reproduce these results, I'm attaching two inlists. One produces
the evolution up to ZAMS and the second is designed to take it from
there up to the core collapse (CC) stage. I'm using version r15140 of
MESA.

At this point, I can use some help from MESA experts. What I'm looking
for is help in creating a basic inlist without any advanced effects
that can evolve the star to the core collapse stage. Advanced effects
can come later once I have a working solution for massive pop III
stars.

I was hoping to reproduce the results of Yoon, Dierks, & Langer (2012)
shown in their Fig. 1 & 2. They show the evolution only up to He core
depletion. In my case, I need to go beyond this to the core collapse
stage with and without rotation.

I'll really appreciate any help that you can offer. Please let me know
if you need any further info from me and forgive me if I haven't been
so clear in describing the problem.

Thanks,
Ramandeep
-- 
Ramandeep Gill
Postdoctoral Fellow
George Washington University
The Open University of Israel
http://www.ramandeepgill.com
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