PNe

I'm running the updated problem module from Jonathan. Many thanks.

Initial wind phase, 7-level AMR. Plots of density (g/cc), temperature (K) and Mach number. ​frames

From last meeting with Adam, Luke and Zhuo, we came up some options to explore:

• gamma = 1 (still use the ideal gas EoS?)
• widen box — make it a cube, run on lower resolution
• apply DM cooling where the shocked gas temperature is greater than 10000 K
• wide/narrow angle jets
• precessing jet — need Nozzle module

Things to look into:

• opacity in the CE ejecta vs. the out-flowing wind.
• as temperature goes up and density goes done, what happens to opacity?
• metal cooling and other cooling curves in the code

Summary of recent work

1. Continued to write/edit energy paper
2. Plots for energy paper
3. New longer movie of AGB run

Conferences

1. Grand Challenges in Stellar Physics: Pulsating Stars in the Universe
   • Apr 1-5, 2019
   • Nice, France
   • website doesn’t seem to be up yet
2. The Deaths and Afterlives of Stars
   • Apr 22-24, 2019
   • Space Telescope Science Institute, Baltimore
   • ​http://www.stsci.edu/institute/conference/spring2019
   • Registration fee: $200
   • Deadline for abstract submission: Dec 15 if want to be considered for financial assistance
3. New Perspectives on Galactic Magnetism
   • June 10-14, 2019
   • Newcastle upon Tyne, UK
4. The Beginnings and Ends of Double White Dwarfs
   • Jul 1-5, 2019
   • Dark Cosmology Centre, Niels Bohr Institute, Copenhagen, DK
   • ​https://dark.nbi.ku.dk/the-beginnings-and-ends-of-double-white-dwarfs/
5. The Role of Outflows in Compact Binaries
   • Jul 1-3, 2019
   • Amsterdam, NL
   • ​https://outflows2019.com/

Tentative plan:

• First trip: Attend #2 (within USA)
• Second trip: Attend #3 and #4 (or #5) (Europe)

Energy paper

Overleaf: ​https://www.overleaf.com/project/5bd20d99379a851a13bfd103

New 2D plots I am using to write the section on the spatial analysis: ​http://www.pas.rochester.edu/~lchamandy/CE_papers/Energy/en_fig.pdf

Medium resolution AGB run (one less level of AMR than fiducial RGB run)

​Face-on density (zoomed in) (Run 164, m2=1 Msun)

Papers on CE simulations involving AGB primaries

• ​Sandquist et al. 1998
• ​Staff et al. 2016

Parameter Space Paper

Submitted. Need to get password for one of macs to get data for movies to upload to YouTube. Also need to make list of people to send to.

Radiation Pressure

7 additional frames finished. VisIt is having problems drawing the Mach contour the first time (works on redraw) — any thoughts?

There may be a slight bulge starting at the planet again, but it's still too early to say definitively.

AMR line transfer

Jonathan and I had a productive meeting two Wednesdays ago. I should be able to sit down and get a functional version this week.

Project Statuses

• Radiation Pressure
  • Outline of ​paper
  • Need to make a few more plots for high Lyman flux case, once it's completed (early December?)
  • Will address Eric's email, as well - measure speeds of blowoff at a variety of points along side and compare to energy requirements
• AMR line transfer
  • Sketch of code written, significant modifications required
• Charge exchange
  • Next will be stellar wind, no ionizing flux, to see effects of just mixing
• HD209458b
  • High ionizing flux - effect on mass loss rate/wind structure

Updated Plan from ​plans of october

Three 4-Bay NAS DiskStations with Twelve 8TB or 10TB hard drive

1. Can use one DiskStation and Four hard drives for archiving data and turn it off
2. Can connect Two or Three together as JBOD for saving data with redundancy.
3. Fast order&delivery: can order directly from newegg (without with p-card or through the system)

Plan A: ~$3600 for 96TB

Plan B: ~$4600 for 120TB

Total Energy with contours

Absolute value of total energy; Density Contour; orbital plane
​https://www.pas.rochester.edu/~yishengtu/CEE_gp_meeting_11122018/Density%20contour/With_density_contour_En/Etot_gas_abs/

Normalized energy; Density Contour; orbital plane
​https://www.pas.rochester.edu/~yishengtu/CEE_gp_meeting_11122018/Density%20contour/With_density_contour_En/Etot_gas_normal/

Normalized energy; Absolute value of total energy Contour; orbital plane
​https://www.pas.rochester.edu/~yishengtu/CEE_gp_meeting_11122018/En_abs%20contour/Etot_gas_normal/

Absolute value of total energy; Density Contour; perpendicular to orbital plane, through particles
​https://www.pas.rochester.edu/~yishengtu/CEE_gp_meeting_11122018/Density%20contour/With_density_contour_En_else_plane/Etot_gas_abs/

Normalized energy; Density Contour; perpendicular to orbital plane, through particles
​https://www.pas.rochester.edu/~yishengtu/CEE_gp_meeting_11122018/Density%20contour/With_density_contour_En_else_plane/Etot_gas_normal/

Kinetic, Internal and potential with Contour

Kinetic energy; Density contour and E=0 Coutour; orbital plane

• D100: ​https://www.pas.rochester.edu/~yishengtu/CEE_gp_meeting_11192018/E_kin_abs/D100.gif
• D400: ​https://www.pas.rochester.edu/~yishengtu/CEE_gp_meeting_11192018/E_kin_abs/D400.gif

Internal energy; Density contour and E=0 Coutour; orbital plane

• D100: ​https://www.pas.rochester.edu/~yishengtu/CEE_gp_meeting_11192018/E_int_abs/D100.gif
• D400: ​https://www.pas.rochester.edu/~yishengtu/CEE_gp_meeting_11192018/E_int_abs/D400.gif

Kin+Int energy; Density contour and E=0 Coutour; orbital plane

• D100: ​https://www.pas.rochester.edu/~yishengtu/CEE_gp_meeting_11192018/E_kin_and_int_abs/D100.gif
• D400: ​https://www.pas.rochester.edu/~yishengtu/CEE_gp_meeting_11192018/E_kin_and_int_abs/D400.gif

Potential energy; Density contour and E=0 Coutour; orbital plane

• D100: ​https://www.pas.rochester.edu/~yishengtu/CEE_gp_meeting_11192018/E_tot_pot_abs/D100.gif
• D400: ​https://www.pas.rochester.edu/~yishengtu/CEE_gp_meeting_11192018/E_tot_pot_abs/D400.gif

Combined

• 4 Horizontal: ​https://www.pas.rochester.edu/~yishengtu/CEE_gp_meeting_11192018/Kin__Int__KinInt__Pot/D100H.gif
• 2 Horizontal, 2 Vertical: ​https://www.pas.rochester.edu/~yishengtu/CEE_gp_meeting_11192018/Kin__Int__KinInt__Pot/D100S.gif

The number of radiative force is,

f_{rad}/f_{g}

The first row is the top views, the second row is the side view.

Planetary Nebula Simulation

1. Protection issue
   • MinDensity = 1d-100 in density protection
   • Regenerated frame 0, running the initial wind phase
   • Now temperature drops below the MinTemp(=1d-10) in pressure protection
   • See ​plots

Mach number (did something wrong?)

2. Cooling (Gamma = 1)
   • Need to learn terms in a(5,128) and b(5,192) matrices in problem modules.
   • Read in quantities from SPH output and mapped to Info%q(i,j,k,1-5). See quoted code below.
   • a,b matrices: 1-density, 2-v_x, 3-v_y, 4-v_z, 5-not sure
   • Info%q: 1-density, 2-p_x, 3-p_y, 4-p_z, 5-energy density
   • Missing gamma?

select case(info%level)
    case(0)
        do k=1,128
           do j=1,128
              read(195,*),a(1,:)
              read(196,*),a(2,:)
              read(197,*),a(3,:)
              read(198,*),a(4,:)
              read(199,*),a(5,:)
              if (j.ge.57.and.j.le.72) then
                  do i=1,16
                      Info%q(i,j-56,k,1)=a(1,56+i)/rscale
                      Info%q(i,j-56,k,2)=a(1,56+i)*a(2,56+i)/rscale/velscale
                      Info%q(i,j-56,k,3)=a(1,56+i)*a(3,56+i)/rscale/velscale
                      Info%q(i,j-56,k,4)=a(1,56+i)*a(4,56+i)/rscale/velscale
                      Info%q(i,j-56,k,5)=a(1,56+i)*(a(5,56+i)+0.5*(a(2,56+i)&
                      *a(2,56+i)+a(3,56+i)*a(3,56+i)+a(4,56+i)*a(4,56+i)))/pscale
                  end do
              end if
           end do
        end do

$\gamma_{7_1} = \frac{5}{3},\,\, \gamma_{7_2} = 1\\ e_{T1}=\gamma_{7_1} P_1\\ P_1 = \frac{e_{T1}}{\gamma_{7_1}}=P_2=P\\ e_{T2} = e_{T1} \frac{\gamma_{7_2}}{\gamma_{7_1}} = \gamma_{7_2}P\\ E = e_{k1}+e_{T2}$

3. AMR
   • Trying on different qTolerance

Project Statuses

• ​Parameter space paper
  • Ready to resubmit
  • Need to retrieve data for some movies, then to be posted on YouTube
  • Waiting on John to submit to arXiv
• Radiation Pressure
  • Outline of ​paper
  • Need to make plots as listed
  • Need a few more frames of high flux - keep running out of memory, currently trying 8 GB/CPU
• HD209458b
  • High ionizing flux got 7 frames in 5 days, so could probably see changes in ~1 month
• Charge exchange
  • Believe I have stellar wind on the grid successfully
  • Need to test charge exchange now
• AMR line transfer
  • Sketch of code written (see ​previous blog post)
  • Jonathan and I are going to discuss this week sometime

HD209458b

Here's frame 7 of the high ionizing flux run. You can see the hotter wind material bubbling out into the Hill sphere.

Charge Exchange

Stellar wind appears to be successfully on the grid.

Initial:

Final (link to movie):

Planetary Nebula Simulation

Current status and things to be done

1. Tuning AMR
   • Refinements triggered on density gradient.
   • Restarted from high-momentum run02 frame with jets out.
   • Ran 5-level AMR (figure below). However, the outflow was turned off.
   • Current run starts from the same frame with 7-level AMR, and outflow turned on. The job is running on 120 nodes with 20-gb memory per node. It has been running for 4 hours (as I'm writing this blog) to generate 1 frame. Need better tuning on qTolerence, or reduce AMR level.
   • Next, start with no jets and then turn on the outflow. See if AMR capture the jets as we want.

2. Resolution on cavity walls
   • Issues on pressure and density protection. (tbd)
   • Turn on outflow after initial-wind fills the entire simulation domain.

3. Gamma = 1 (Cooling)
   • Set gamma_7 = 1.001 in the code. (where exactly?)
   • Generate Frame0: Read in SPH results (pressure, kinetic and thermal energy, gamma = 5/3), keep pressure fixed, calculate new thermal energy with gamma = 1.
     $\gamma_{7_1} = \frac{5}{3},\,\, \gamma_{7_2} = 1\\ e_{T1}=\gamma_{7_1} P_1\\ P_1 = \frac{e_{T1}}{\gamma_{7_1}}=P_2=P\\ e_{T2} = e_{T1} \frac{\gamma_{7_2}}{\gamma_{7_1}} = \gamma_{7_2}P\\ E = e_{k1}+e_{T2}$
   • Criteria, say, apply cooling if v > 100 km/s ?

level 5 mesh on 5-level AMR

temperature

Taken at the beginning of the simulation and just before/after turning on the fast wind.

High momentum run 01	High momentum run 02	Initial Wind
InterpOpts = 0	InterpOpts = 1	InterpOpts = 1 , and no fast wind

​Movies and ​Graphics

7-level AMR run returns the following error

bhc0074.bluehive.circ.private:UCM:2a62:11a41700: 520618407 us(520618407 us!!!): dapl async_event: DEV ERR 10
bhc0074.bluehive.circ.private:UCM:2a5a:3db57700: 521043336 us(419038 us): dapl async_event: DEV ERR 9

density and pressure protections in physics.data

!================================================================================
! Density Protection Options
!================================================================================
lRestartOnDensityProtections = .false.  ! Do density protections trigger restarts?  [.false.]
lTrackDensityProtections = .false.      ! Track density protections [.false.]
iDensityProtect  = 0                    ! 0-Set to MinDensity, 1-Set to minimum nearby density, [2]-Average nearby densities
iMomentumProtect = 1                    ! 0-Conserve momentum, 1-Set to zero, [2]-Average nearby velocities
MinDensity       = 1d-15                ! Minimum computational density before protection is triggered [1d-10]

!================================================================================
! Pressure Protection Options
!================================================================================
lRestartOnPressureProtections = .false. ! Do pressure protections trigger restarts? [.false.]
lTrackPressureProtections = .false.     ! Track pressure protections [.false.]
iPressureProtect = 0                    ! 0-Set to MinTemp, 1-Set to minimim nearby pressure, [2]-Set to average nearby pressure, 3-Set to minimum nearby temperature, 4-Set to average nearby temperature
MinTemp          = 1d-10                ! [1d-10] minimum allowed temperature for the system in Kelvin before protection is triggered

!================================================================================