[Mesa-users] Fwd: 100 M_sun non stripped progenitor, Resulting SN, a normal type IIP or PPISN?

Tue Aug 17 16:07:03 UTC 2021

Dear sir,

Many thanks for your reply. It cleared many things for me. I would be very
grateful to you if you suggest ( any reference on ) how to check the
explodability of a model on the verge of core-collapse? I could see (please
see the attached figure) that the central temperature and density near
Fe-core infall have reached in excess of 10^10 K and 10^10 g/cm^3
respectively which are suitable conditions for the core to collapse.

One more thing, As I mentioned in my previous mail, the mass of the core
obtained corresponding to the three energies ( *0.5d+51,* *1.0d+51 and, *
*1.5d+51*) are * 41.135, 38.050, and 31.239 M_sun *respectively, So should
we expect that these SNe explosions would result in the formation of black
holes?

Please provide your valuable suggestion.

With thanks and regards,
Amar

------------------------------
*From: *pamarca at gmail.com
*To: *amar at aries.res.in
*Cc: *mesa-users at lists.mesastar.org, Amararyan941 at gmail.com
*Sent: *Monday, August 16, 2021 5:26:24 PM
*Subject: *Re: [Mesa-users] 100 M_sun non stripped progenitor, Resulting
SN, a normal type IIP or PPISN?

Hi Amar,

I can provide some answers to your points 2 and 3.

2) In your simulations you are taking the model at iron core collapse and
modelling a supernova by excising the core, injecting a specified amount of
energy and putting in some nickel. The pulsational pair-instability process
would precede iron core collapse. I would suggest you check the late
evolution of central temperature in your models and compare it to the upper
panels of figure 3 in Woosley et al. (2017). Evolution might resemble those
cases which are weak pulsations that wont result in much mass loss (and for
a hydrogen rich envelope, you might not even have shock breakout from the
pulses before iron-core collapse). From what you describe it is not
surprising that you get results resembling a type IIP supernovae, as you're
modelling the evolution past iron core collapse as an iron-core collapse
supernovae, independent of the evolution prior to that. Beware that its not
even certain such systems would undergo a supernova at iron-core collapse.

3) The ppisn example is not meant to model a light curve. The end model you
get from it is also just a model at iron-core collapse, so the ppisn
evolution will already have happened. If you are only concerned with the
models you mentioned you can likely still use the example_ccsn_IIP test
case. This will not give you the ppisn light curve but instead a light
curve associated to a potential iron-core collapse supernova at the end of
its life. If you want to construct light curves for pulsational
pair-instability supernovae that is a much more complex thing to do with
MESA+stella at the moment, and it would require an important amount of work
to setup.

Cheers

On Fri, Aug 13, 2021 at 2:43 PM Amar Aryan via Mesa-users <
mesa-users at lists.mesastar.org> wrote:

> Dear MESA troubleshooting team,
>
> Please provide your valuable suggestion to the queries in my previous
> email. I shall be highly thankful for any suggestions or comments.
>
> With best regards,
> Amar
>
> ------------------------------
> *From: *amar at aries.res.in
> *To: *"mesa-users" <mesa-users at lists.mesastar.org>
> *Cc: *"Amararyan941" <Amararyan941 at gmail.com>
> *Sent: *Sunday, August 8, 2021 7:52:02 PM
> *Subject: *100 M_sun non stripped progenitor, Resulting SN, a normal type
> IIP or PPISN?
>
> Dear MESA troubleshooting team,
>
>                   OS : Ubuntu 20.04
> MESA Version : 11701
>
> I am trying to evolve a non stripped 100 M_sun model having Z=0.01, up to
> the onset of core-collapse, and then calculate the corresponding light
> curve and velocity evolutions. I have made the following changes in the
> default test directory :
>
> In inlist_common :
>
> convective overshooting parameters, *f= 0.001* and *f0 = 0.004*
>
> In inlist_to_lgT9.9 :
>
> log_center_temp_limit =* 9.85d0  *(because Fe-core infall limit is
> reached near this temperature)
>
> Further, the shock is evolved using the example_ccsn_IIP directory with a
> few nominal changes :
>
> In inlist_infall :
>
> remove_initial_center_by_entropy = *4.01 *.
>
> In inlist_edep :
>
> inject_until_reach_model_with_total_energy = *1.5d+51* (also with
> *0.5d+51* and *1.0d+51*)
>
> In inlist_shock_part5 :
>
>   x_ctrl(12) = *0.1* !Nickel mass
>
> The mass of the core obtained corresponding to these three energies are *31.239,
> 41.135, and 38.050 M_sun *respectively!
> The model is well evolved and the light curve calculations are done using
> STELLA. Here are the light curve and velocity evolutions obtained :
>
>
> Now, I have a few doubts :
>
> 1) Although the light curves are produced up to 400 days but the
> photospheric velocities (plotted using *mesa.swd.ph <http://mesa.swd.ph>*
> file) are produced only up to 170 days. What should I do to obtain the
> velocity evolution of late phases?
>
> 2) A bit scientific one!  For helium cores more massive than about 30
> M_sun, post carbon-burning stages are, initially at least, unstable
> (Woosley et al. 2017) and the star itself is unstable (condition of a PISN
> or PPISN). So, for our case also, *should the model result in a PISN or
> PPISN?* But our calculations seem to indicate a normal type IIP SNe. I am
> in huge doubt. Please provide your valuable suggestion.
> 3) I tried to run the default *ppisn* directory. The calculation
> successfully proceeded and generated a *final.mod* file. But how can I
> extract the light curve and  velocity evolutions? Do I need the use the
> example_ccsn_IIp directory here also?
>
> 4) Recently, I installed MESA Version 15140 and tried to make stripped SN
> progenitors. But unlike MESA version 11701, I do not find artificial
> stripping option (*mass_change = -1d-4* in *inlist_remove*). So, please
> suggest how can we make stripped progenitors in latest versions of MESA?
>
> I am sorry for disturbing on a holiday. Please suggest and provide your
> valuable suggestions.
>
> Thank you in advance for any sort of suggestions and comments!
>
> With regards,
> Amar
>
>
>
>
> _______________________________________________
> mesa-users at lists.mesastar.org
> https://lists.mesastar.org/mailman/listinfo/mesa-users
>
>

-- 
Pablo Marchant Campos
M.Sc on Astrophysics, Universidad Católica de Chile
PhD on Astrophysics, Argelander-Institut für Astronomie, Universität Bonn
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