Calculation Logs

= Calculation Log =

NOTE: Figures and data are basically stored in Dropbox.

PPN
- 10/9-10/2019: Calculated overproduction factor (abundance ratio to the case with the Kappeler 1994 rate) as per request of Greg and Grisha. 5 solar mass with solar system metallicity (asplund). Trajectory.inpu was obtained from star.log. See 191010. The results do not agree much with Heshani's NEWTON calculations. But I checked trajectories, etc, carefully, so my calculations should be ok.

- 10/12: Since I found the calculations above are not right (used Z=0.01 Asplund 2005 abundance), I recalculated with Z=0.02 abundance files (GN93). The results still don't match with Heshani's calculations, but they changed quite a bit from Z=0.01 ones.

- 10/13: Run XRB examples.Learned many heavy p-rich nuclei are actually produced by successive (p,g) on stable heavy nuclei (not simply started from light stable nuclei).

- 10/27: Run XRB examples. Tested changing a reaction (59Cu(p,g)) by factor of 100 (in ppn_physics.input) and see if the abundances are changed. I confirmed it does. However, only neighborning nuclei are changed and no effect on lighter or much heavier nuclei. This is because I'm running in single zone and energy generation is not affected by this reaction change (which should be a lot; see Cybert APJ 2016). Also I wrote some scripts in analysis directory.

MPPNP
- 10/10-14/2019 (GCA): Calculated 5M Z=0.02 from the Canfar hdf5 data. 22Ne(a,n/g) rates are (probably) set to Kappeler1994??. Because PPN results didn't agree with Talwar or Heshani either, so I just hoped MPPNP might improve the disagreement.

- 10/17-22/2019 - (WENDI) : Calculated 5M Z=0.02 from the Canfar hdf5 data. 22Ne(a,n/g) rates are set to Longland2012.

- 10/17-21/2019 - (GCA) : Calculated 5M Z=0.02 from the Canfar hdf5 data. 22Ne(a,n/g) rates are set to Talwar2016.

- 10/18-19/2019 - (GC-Master) : Calculated 5M Z=0.02 from the Canfar hdf5 data. 22Ne(a,n/g) rates are set to Massimi2015.

- 10/20/2019 - (GC-Master) : Calculated 5M Z=0.02 from the Canfar hdf5 data. 22Ne(a,n/g) rates are set to Kappeler1994 (to check 10/10-14 run is truly Kappeler1994).

- 10/24-25/2019 (GCA): Recalculated 5 M Z=0.02 (initially 10/17-21) because some outputs (hdf5) have bad data (missing some cycles; 385001, 435001, ect). So tried by just running these cycles.

- 10/30-31/2019 (GC-MASTER): 25M Z=0.02 from the Canfar hdf5 data. To see s-process impact on massive stars. 22Ne(a,n/g) rates set to Talwar2016.

MESA
- 6/23/2019: Calculated neutron abundance in 25 solar mass stars. See 190623

- 10/9/: Calculated 5 solar mass AGB (based on 7M_prems_to_AGB). Checked HR diagram and T-rho curves, etc. Confirmed the T-rho trajectory agrees very well with Canfar data's trajectory.

- 10/11: Calculated nova and 25M_pre_ms_to_core_collapse from test_suite on WENDI (just for curiosity). Nova trajectory seems very different from XRB trajectory on PPN examples. Also, 25M trajectory is not similar to 25M_ccsn on PPN examples (but this is probably PPN shows C or He burning's trajectory).

- 10/12: Calculated C13_pocket and He_core_flash from test_suite on WENDI (for curiosity).