Posts for the month of December 2021
CE EOS Simulations
Computing
- Allocation on Frontera ends on Dec. 31 — update?
- Parallel HDF5 (currently only being used for post-processing)
- Bug has been identified and debugging ongoing (Jonathan)
Energy conservation
- Tested new poisson.f90 designed to explicitly conserve energy (though not yet including particles), as in Jiang+13.
- Used low resolution CE run with periodic boundary conditions (so that flux of energy through boundaries does not change total energy in domain)
- Found that energy conservation is worse than with the original poisson.f90, not better.
- This means that there is a bug in the new poisson.f90 (could it be something obvious?)
EOS Runs
- Computed volume integrated mass and released energy for Run 271, using Python, plotted, and made pdf file. Includes only 3 frames (frame 0, 100 and 200).
- See these notes.
Runs for the paper
The plan is to compare 3 runs which are identical except for the EOS:
- Run 277: MESA EOS (completed up to frame 170 and will go as far as energy conservation allows, maybe frame 300
- Run 282: Ideal gas gamma=5/3 EOS (completed up to frame 33 and will go up to frame ~300).
- Run 283: MESA EOS with recombination energy removed from EOS tables (not yet started, will go up to frame ~300)
We are also doing a high resolution run for a convergence study:
- Run 276: MESA EOS with maxlevel increased by 1 (completed up to frame 47 and will go up to at least frame 65)
Next steps
- Complete all runs and do basic analysis (separation vs time, energy conservation)
- Redo unbound mass vs time plots to include only envelope gas (exclude ambient) — can wait for runs 277 and 282
CE EOS
Computing
- Allocation on Frontera ends on Dec. 31
- Parallel HDF5 (currently only being used for post-processing)
- Bug has been identified and debugging ongoing (Jonathan)
EOS Runs
- Continued analysis of Run 271:
- New PLOT of energy terms that includes recombination energy
- Volume integrated mass and energy released for the products of the various ionic transitions, for 3 snapshots (t=0, 23 d and 46 d)
- Same, but divided into gas that is unbound and gas that is bound (at time t)
- This analysis so far only on IDL (plot to screen)
Next steps
- Do the above analysis (volume integrated mass and released energy for each species) but now for all simulation frames of Run 271, using Python
- Continue with production runs (Stampede2 and Frontera)
- Compute ambient unbound mass and subtract from total (as Amy has now done for jet runs)
CE (EOS)
Computing
- Allocation on Frontera ends on Dec. 31
- Need to ask for extension ASAP
- Could also request transfer SUs to Stampede2 if necessary
- https://portal.xsede.org/allocations/managing includes info from XSEDE about extension and transfer requests
- Parallel HDF5 (currently only being used for post-processing)
- Bug has been identified and debugging ongoing (Jonathan)
EOS Runs
- Slices comparing density of tracers for original ionization state with density of gas with a given ionization state at time t
- See these notes.
- Trying to improve energy conservation — Goal is to get simulation up to >100 days (c.f.~Ohlmann+16: 125 days; Prust+Chang19: 240 days)
- Do this by testing adding refinement in different ways:
- One extra AMR level
- Larger region for AMR level 4
- Larger region for max AMR level
- Do we work to implement the new algorithm that includes gas potential energy in the explicit energy conservation (though not particle-gas potential energy) or do we carry on with what we have?
- Do this by testing adding refinement in different ways:
- Energy conservation normalized to initial energy of star, not including recombination energy:
Figure
- So continuing to 100-150 days and staying <10% should be possible, particularly if we reduce softening radius 2-3 times…
- Currently running a test where the highest AMR level refinement region is enlarged…results very soon
Next steps
- Production runs on Frontera?
- Compute ambient unbound mass and subtract from total (as Amy has now done for jet runs)
- Compute total recombination energy of each species (e.g. HII, HeIII) as a function of time
- Compute total recombination energy of each species (e.g. HII, HeIII) as a function of time for bound and unbound mass separately
- This will tell us whether recombination energy is being released into bound gas (where it can be "useful") vs. unbound gas (where it cannot), c.f. Fig. 1 of Paper II
- Some version of Figs. 9 and 10 of Paper IV that includes recombination energy
Fermi Project Update December 2021
Goal: find technology as a function of galactic orbital radius
- Find density as a function of radius
- Get technology as a function of density
2a. Recreate surface plot made with Jonathan (with )
- f is the fraction of systems that are settleable
- is the normalized density of settleable systems within probe range
- is the settlement civilization lifetime
- X is the local fraction of settled systems to total systems
2b. Rerun the same parameter sweep but make
2c. Do some lineouts to get technology and X as function of density
- Interpolate to get density as a function of radius. (not entirely sure how to do this one)