Update 08/05

CEJet

Current run on Stampede

In queue, expected start time is tomorrow morning at 6:30.

Same as the 1st run, but with all the total quantities defined as the current CE settings. Use refinement radius as CE model B in paper II, 4d12 for frames 0-45.

Parameters of the Jet

  • mass loss
2 1000 1e5
0.2 100 10 000
2e-3 1 100
2e-5 0.01 1
  • launching radius
jet radius (cells) jet radius
16 2.25 (=1 base grid)
  • speeds
jet radial speed (km/s) Keplerian speed (km/s) Q (fraction of Keplerian speed) approx. rotation speed (km/s)
430.75 430.75 1 1 0.5
  • others
collimation angle (half) (degrees) index (exponent of collimation) jet temperature (K) lcorrect (conservation)
15 1 30 000 T

—-

PN

Flows during initial wind period

The total amount of gas flow into the wind radius is . This amount of gas has been removed from the simulation. The inflow through the outer boundaries is almost negligible (1e-7 solar mass).

This means almost half the initial gas (0.4 solar mass) has been removed. There is a stream of inflow through the funnel with a slow speed, but since it’s at the region of highest density, it takes a lot mass in.

​velocity plots

​density plots

​python notebook

​test without IW

The SPH CEE simulation contains

  • Primary of mass 0.88 M_sun, where
    • the core mass is 0.392 M_sun, and
    • the envelope is 0.488 M_sun
  • Secondary (point particle) of mass 0.6 M_sun
  • so the amount of gas for us to start the PN simulation is about the envelope mass of the SPH primary

Frame 0 has

  • total mass of the gas about 16 solar mass — M_tot =16.136 M_sun
  • if set a density threshold at 1e-8 g/cc, then
    • the high density region sum up to — M_high=15.712 M_sun, while
    • the low density region sum up to — M_low = 0.424 M_sun

NOTE

  1. The density threshold is chosen as such, because since frame 1, the maximum density in the simulation is on the order of 1e-8 g/cc.
  2. The total mass of the low density gas is about right to the total amount of gas we start with.
  3. The high density region is produced from mapping the SPH data onto the AMR grids. The SPH data has local maximum density on the order of 0.1 g/cc, while frame 0 has local maximum of 0.05 g/cc.
  4. The mass of the high density gas is confined at a point close to the simulation center with a radius of 7.6 R_sun (about the size of our finest grid). These 4 extremely high density grids are within the wind initialization radius, so once the simulation starts they are removed, and won't affect the simulation any further.
  5. I interprete this 16 M_sun region as the final location of the binary core from the SPH simulation. Maybe the core is more confined in the SPH simulation but spreads out in AMR grids and produce this artifect of a huge amount of mass.

Between Frame 0 and Frame 1, there are few sources and sinks of mass:

  1. Sink - Lowering the floor density for density protection, the maximum effect has the change of -1.4e-3 M_sun
  2. Source-Sink - carving out the central region and replace with a 1 solar mass point particle and fill the rest of the region with initial wind density.

From Frame 1 to Frame 149 (before fast wind starts):

  1. Source - inflow from the outer boundary of the simulation. During the entire initial wind period (3000 days), the total amount of inflow gas is 1.11E-7 M_sun, almost negligible
  2. Sink - gas flows into the wind initilization radius will be removed from the simulation, and the total change is -0.19 M_sun

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