Posts for the month of February 2019

Update 02/25

PNe

  • I have a new reservation on BlueHive started this morning at 8. Currently running the two cooling models: High-momentum at frame 189/300, and low momentum at frame 231/300.
  • Need to extend the time for those cooling case to evolve longer. The morphology hasn't grow far from the core area, and in low-momentum case, the jet hasn't propagate through the funnel yet.
  • The non-cooling, high-momentum ran into a resolution problem at frame 212. Redoing those frames now.
  • Non-cooling, low-momentum case, currently at frame 259/300. I'm thinking of redo some later frames to keep the high resolution area cover the entire PN lobes.

CEJet

  • Did a test run with no secondary mass (run008-amy).
  • I made script for measuring total mass and mass-loss rate. in run008, the rate mass being added is not a constant.
  • Schedule a paper discussion next week.

others

  • the MESA summer school

Update 02/18

​non-cooling

​cooling plots

Update 2/18

Radiation Pressure Paper

Believe it's nearly done. Could use some help with the results comparison section and the punchiness of the conclusions, and there's one more measurement I need to make (will likely have to wait until after my qual).

Next Steps

  • Finish AMR line transfer
    • Believe I have a working algorithm, just need to finish implementing it
  • Charge exchange
    • Will run just stellar wind, no ionizing flux, to see effects of mixing only
    • May be able to run later this week
    • Think it would be useful to run HD209458b with just stellar wind as well as charge exchange, both for comparison with Cherenkov et al. and to separate the effects of each (under the assumption that John's results may not be representative of the results for the significantly different planet)
  • What next? Spherical line transfer?

Accretion Disk Update

I have been working on simulating an accretion disk embedded in the center of an AGB star. Previous simulations have utilized a sink particle that relieved thermal energy and led to very high accretion rates. Our sink particle is set to “NOACCRETION ”.

The box size is 10e11 cm

Accretion disk has Radius of 2*10e10 cm and Height of 5*10e9 cm

Animations of the density (Top Down):

https://guidarellig.github.io/RhoTop.mpg

and Temperature (Side):

https://guidarellig.github.io/TempSide.mpg

My first attempt to look at the accretion rate was to define a momentum flux with:

p = rho*v

dQ = p dot dA

Summing dQ over a surface yields the flow rate through that surface, I did this with spheres. The next animation shows the accretion rate in solar masses per year (y-axis) through spheres of different radii (x-axis) over time <note: positive value correspond to outward flow>:

https://guidarellig.github.io/AccretionZoomed.mpg

For a general sense of the direction of flow this animation shows red as outward flow and blue as inward:

https://guidarellig.github.io/Check.mpg

To represent accretion clearly Luke and Eric suggested calculating the total mass as a function of time. (it is much better)

The total mass inside a sphere of radius 0.4e10 cm:

https://guidarellig.github.io/MassInsideSpherep4R.png

Mass inside shells of constant thickness (0.05e10cm) and different outer radii:

https://guidarellig.github.io/MassInsideShellsp4R.png

Mass inside cylinder of disk height and radius 0.75e10 cm:

https://guidarellig.github.io/MassInDiskp75R.png

Mass inside hollow cylinder of disk height, constant thickness (0.125e10cm) and different radii:

https://guidarellig.github.io/MassInRingsp75R.png

Update 02/11

PNe Simulation

http://www.pas.rochester.edu/~yzou5/PNe_graphics/20190211_IW.png

  • Production runs: initial wind runs to 168/300 frames. Estimated wall time remaining is 10 days, but I've doubled the cores (120) and should take less than that.
  • Need to reserve nodes on Bluehive for the rest (high-/low-momentum, adiabatic and cooling for each).
  • Low-momentum, refinement issue solved by reducing mintracer to 0.0001 (0.1 originally)
  • cooling, issue with tracer density when triggering temperature protection. Should be a quick fix. ​plots
  • Inner boundary conditions, look for zero pressure gradient at the inner radius where outflows start.

Moving on

  • Begin working on Toro's book
  • Pick up recombination

ProtectOutfowTemp subroutine added on Jan 31

SUBROUTINE ProtectOutflowTemp(pos,t,dt,q,Ghost)
  USE GlobalDeclarations
  REAL(KIND=qPREC), DIMENSION(:), INTENT(IN) :: pos
  REAL(KIND=qPREC), DIMENSION(:), INTENT(INOUT) :: q
  REAL(KIND=qPREC), INTENT(IN) :: t, dt
  LOGICAL, INTENT(IN) :: Ghost
  if (q(particle%outflowobj%itracer) > 1e-4*particle%outflowobj%density) then
     q(iE)=max(q(1)*FloorTemp/TempScale, q(iE))
  end if
END SUBROUTINE ProtectOutflowTemp