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

[amar at aries.res.in]

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 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 



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