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

Mon Apr 5 23:14:31 UTC 2021

Hi Rob,

Thanks for your input on how to make the Kippenhahn diagrams in MESA.
It was very helpful.

I'm attaching below the results for the 60 M_sun model that was run
using v15140. All files are labeled with the MESA version used. To
remind you, this model crashes during core Carbon burn due to the
timestep becoming too small. The attached figures may provide more
insight into what might be going on.

I also took the time over the last few days to experiment with other
published inlists to see if they can be applied to my problem. I found
one prepared by Matteo Cantiello for the paper Perna, Lazzati,
Cantiello, 2018, ApJ, 859, 48. In that work, they evolve massive [40
M_sun] stars with Z = 1e-5 from zams to iron core formation using
MESA_v9793. First I tried the same inlist with the current MESA
version, it didn't work due to several changes to the code. I was able
to install v9793 successfully which I then used to reproduce Matteo's
results from that paper. In the next step, I tried to lower the
metallicity. I was able to get a solution for Z = 5e-7 until the
formation of the Iron core, which I also attach [notice the different
version v9793 in the attached figs].

The problem here was that with the adopted mass-loss prescription due
to radiative winds [Dutch with scaling factor 0.8], the star loses too
much mass [from 60 M to 21 M] even with such low Z. Other works that
evolve Z=0 stars find only minimal mass loss due to rotation. Lowering
the Dutch scaling factor or turning it off completely crashes in MESA.

If we can find a way to avoid very small time steps then some progress
can be made. Let me know your thoughts on this. Another point that's
worth considering is the mass loss prescription. Many Z=0 works use
the Kudritzki model which is not one of the options in MESA and so I
couldn't use it. Perhaps there's another way to implement it.

Best,
Ramandeep

On Thu, Apr 1, 2021 at 12:53 AM Rob Farmer <robert.j.farmer37 at gmail.com> wrote:
>
> Hi,
> There are python codes available for making kippenhans, but for now the simplest is to let mesa make them for you.
>
> Add:
> mixing_regions 40
> burning_regions 40
> to your history_columns file
>
> and add:
> kipp_win_flag=.true.
> in your pgstar inlist
>
> Rob
>
>
>
> On Thu, 1 Apr 2021 at 01:13, Ramandeep Gill <rsgill.rg at gmail.com> wrote:
>>
>> Hi Rob,
>>
>> Thanks for writing back. Let me first answer your questions and then I
>> can provide some more details.
>>
>> The model fails during Carbon ignition in the core. For your reference
>> I've attached two screenshots of the output just before the code
>> crashes. Fig.1 shows the Carbon fraction with C_cntr = 0.000131 and
>> this the lowest I've obtained with the current setup. The figure also
>> shows the current time step which is very small. The code crashes very
>> soon after this and that's shown in Fig. 2, just to give you some idea
>> of the error messages before it crashes. The time step is being
>> determined by max_increase, and I don't really know what that means.
>>
>> I'll have to look into how to produce a Kippenhahn diagram. A quick
>> search on google revealed that many have written python scripts to do
>> just that. So, I might adopt one of them.
>>
>> Finally, I looked at the MESA instrument paper II, which presents the
>> evolution of a 40 M_sun star with rotation for a low Z = 1e-5. I was
>> able to get the inlist for this paper from MESA marketplace. This
>> seemed like a perfect example for my case. I tried it with the most
>> recent version of MESA, and after fixing a few flags that have been
>> changed in the recent version, I was able to run it. However, it
>> crashed very quickly while core H ignition. Perhaps there's a way to
>> run this example with the latest version. Or I can try to install the
>> same version, if it's still available, that was used for that paper
>> and then run it.
>>
>> Thanks,
>> Ramandeep
>>
>> NB: In my original message I attached inlist_CC but it's missing some
>> flags that initialize the rotation. It's not the inlist that was used
>> to produce the attached HR diagram. So, I'm attaching the proper
>> inlist here. Sorry for the confusion.
>>
>>
>> On Wed, Mar 31, 2021 at 1:20 AM Rob Farmer <robert.j.farmer37 at gmail.com> wrote:
>> >
>> > 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
>> >> _______________________________________________
>> >> mesa-users at lists.mesastar.org
>> >> https://lists.mesastar.org/mailman/listinfo/mesa-users
>> >>
>>
>>
>> --
>> Ramandeep Gill
>> Postdoctoral Fellow
>> George Washington University
>> The Open University of Israel
>> http://www.ramandeepgill.com

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