Documentation - IReNA-NucAstro-QuestionsTools/Supernova-Sunburn GitHub Wiki

We based our work off of preset parameter file Example_CCSN_wind_bliss.par in WinNet, we added neutrino interactions, as seen in the Example_MRSN_nup_process_obergaulinger.par file. We then altered the Ye from 0.2 to 0.9 to see effect on nucleosynthesis and the abundance pattern.

Resources

The edited parameter files can be found in the github repository :

        git clone https://github.com/IReNA-NucAstro-QuestionsTools/Supernova-Sunburn.git

Requirements

  • install WinNet version from 2025

Dependencies

  • Linux, WSL for windows, or Docker for Mac
  • Python 3.10 or newer

How to run

  1. Edit lines 87-97 in the Working_CCSN_wind_bliss.par files to match your directory for the reaction data files. Start with Traj_CPR2_Ye_0.20.txt.

  2. Change line 114 Enuebar to match the value corresponding to the Ye value in the trajectory file. The correct Enuebar value can be found by running Ecalc.py. How this value was calculated can be found in the conclusion page of this wiki.

  3. In main WinNet directory run

    python3 makerun.py -p Working_CCSN_wind_bliss.par -r 'name for output dir'

  4. In /WinNet/bin/movie_script run

    python3 winnet_movie.py -i ../../'name for output dir'/ --save --output='name for movie.mp4' --interval=60

  5. Repeat steps 1-4 for each Traj_CPR2_Ye_*.txt and Enubar

  6. The Plot_me_Ye_range.py can be used to see the output from these, there is some documentation in that code for how to use the plotting code.

Physical Model

Core Collapse SuperNova

Includes:

  • REACLIB-based rates
  • Reverse rates and NSE fallback
  • Weak interactions
  • neutrino interactions EOF

Preset CCSN winds Parameters, Ye = 0.41

https://github.com/user-attachments/assets/fd8c38b8-fddd-47e9-8cce-d365948554c3

Seen above this simulation was used to explore the possibility of the r-process as the Ye fraction is driven towards neutron rich during CCSN[1]. Other papers have varied the Ye in CCSN from 0.4 to 0.65 to explore possible reaction pathways to explain different abundances[1,4,10].

Details on the enviroment

Above are plots discribing the enviroment through the forst 3000 seconds. The Yn quickly drops as the Yp rises. The Ye incorperates all the protons and neutrons in the system, some are trapped in nuclei. You can see the production of heavier nuclei in Yhvy. This being an explosive enviroment both the temperature and density rapidly decrease within seconds, along with the entropy.

The Abundance given the present Ye = 0.41 and only using charged particle interactions. Without the neutrino interactions CCSN only produce up to A ~ 57.

The Ye Shifts up back towards 0.5 as time evolves.