[Mesa-users] STELLA velocity profiles

[Jared Goldberg]

Hi Anna,

I'm a little confused by your question -- are you asking where the forward
shock is? If so, the answer is that the forward-shock has already reached
(or at least come very close to) the surface of the MESA model in the
ccsn_IIp explosion in MESA (see the history file/profileN.data files in
LOGS_part1 through LOGS_part5), and then STELLA tracks evolution after
shock breakout. If this model has CSM, the forward-shock is similarly
probably near the surface of the CSM by the time of maximum luminosity (the
time 0 for these plots) as well. At this point, the reverse shock
(originally generated at the H envelope/He core boundary) IS evolving near
the center (see the left end of the upper left panel), and the opacity
post-shock is primarily electron scattering with the substantial radiative
cooling happening only in the outermost < 0.01 Msun of ejecta for the first
5 days, so it is also not much of a surprise that the opacities are nearly
constant.  So, from my perspective it seems like you're doing everything
correctly.

Cheers,

~Jared

On Mon, Apr 12, 2021 at 5:22 PM Annastasia Haynie via Mesa-users <
mesa-users at lists.mesastar.org> wrote:

> Hi All,
>
> I would appreciate some help identifying where I am going wrong
> in evolving a star in MESA and exploding it in STELLA using the test suite
> make_pre_ccsn_IIp and ccsn_IIp. Currently, I can take the outputs from
> each, create STELLA input files, and using those STELLA runs as expected
> and gives a light curve that makes sense at a glance.
>
> However, when looking into the mesa.day000.X_post_Lbol_max.data files, the
> velocity profiles make it seem as if STELLA is not actually evolving a
> shock front throughout the star. I've attached a plot showing the
> velocity profile for 8 times (in units of days post peak luminosity) along
> with temperature, optical depth, and opacity. In addition to the shock
> being mostly absent from the velocity profiles, the opacity remains nearly
> constant instead of increasing as the material cools.
>
> The plot was created from a STELLA run using the mesa.abn and mesa.hyd
> that come from all of the default settings in make_pre_ccsn_IIp and
> ccsn_IIp, but feeding the "final.mod" file from make_pre_ccsn_IIp  into
> ccsn_IIp instead of using the test case "pre_ccsn.mod", which gives
> different (but not improved) results.
>
> Please let me know if there is a step to using STELLA that I am missing or
> if more information would be helpful to solve this problem.
>
> Best,
> Anna Haynie
> --
> Annastasia Haynie
> PhD Student | GASP Vice President
> Department of Physics and Astronomy
> University of Southern California
> ahaynie at usc.edu | she/her
> _______________________________________________
> mesa-users at lists.mesastar.org
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>
>
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