22Ne an Project

Where should I check the abundance in massive and low (1-3 solar mass) /intermediate (~5 solar mass) mass AGB stars?
- AGB stars: Surface at the end of MPPNP calculations

- Massive stars: At the end of He core burning (inside the core; check the abundance vs mass (radius) plot to see where the core boundary is),at the pre-explosion (i.e., before Si or O burning). Key is where convection occurs (so check Kippenhan diagram).

Research log about 22Ne(a,n) calculations



NuGrid examples based
Note NuGrid PPN is not changed (except for nuclear reaction data file vital.F90).


 * 1) ppn_M25_zsolar_weak_s
 * 2) ppn_M25_zsolar_ccsnshock

Note tried to provide a trajectory.input file from CANFAR data, but PPN gave me an error message (MAX_SUBSTEP is reached). MAX_SUBSTEP is defined in utiliy/source/error.F90, which is related to convergence of Solver. As of 2019/8/24, not sure how to fix this.

Instead, I used trajectory files and initial abundance files in subdirectory (e.g., cases/c or cases/he or cases/center).

Nuclear Reaction Data
physics/source/vital.F90 deals with reaction data. I added Kappeler 1994 data (10/9/2019) and our data (TAMU) (2019 Aug.).

- Talwar2016: Default exists. - Longland2012: Default exists. - Massimi2015: Only upper limit is presented, so UL, Med, LL are all set to the same values. 0.06 - 1 GK are presented. Below and above are taken from M. Wischer data (whatever it is defined in NuGrid). 0.07 GK is interpolated from 0.06 and 0.08 GK data, but this shouldn't have impact. - Kp1994: (Kappeler). - TAMU2019: Given in my PLB paper. 0.1 - 1 GK and below and above are M. Wischer data. Should be calculated with UL ((a,n) UL + (a,g) LL). -

Log
- 8/23/2019: Changed 22Ne(a,n) data among Longland, ND2015 (Talwar), TAMU2019 (Ota), and am trying to see if the calculations are reasonable. It doesn't seem reasonable because Talwar data showed higher heavy element abundances despite that the data has the lower (a,n) rate.