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

[Rob Farmer]

Hi,

The envelopes of massive stars are difficult things to get right. I would
not worry (for now) so much about the envelope, instead worry about what
the star is doing internally. How close to core collapse did your model
get? Has it ignited carbon or later fuels? Try looking at a kippenhan
diagram. If you look over the recent timesteps before the model crashes,
what is limiting the timestep?

Rob



On Tue, 30 Mar 2021 at 22:13, Ramandeep Gill via Mesa-users <
mesa-users at lists.mesastar.org> wrote:

> 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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>
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