Fall Back Disk - Circumbinary Disk

Binary separation = 4 AU

Binary orbital period = 6 years

Simulation temp = 100 K

Primary:

Mass = 1 SM

Quiet phase outflow = 1E-7 SM/yr

Equatorial outflow open angle = 20 degree

Equatorial outflow = 2E-5 SM/yr

It is calculated in this way:

\[\dot{M}=\rho S v\]

\[S=2 \pi r2 \times 2\int_{7\pi/18}{\pi/2} \sin\theta d\theta\]

\[v=\sqrt{v_r2+(\Omega r)2}\]

Equatorial outflow density is increased by 1000 times compared to quite phase, varies with time as the picture below shows, it last for 10 years. The total mass ejected from the equatorial outflow is:

\[M=\delta t \times \dot{M}=2\times10{-4}M_{\odot}\]

Equatorial outflow has angular velocity of:

\[\Omega=1.36294\times10-7 s{-1}\]

This is equivalent to a period of 1.46 years. Since the equatorial outflow is launched at 1 AU, this means .

Secondary:

Mass = 0.5 SM

The simulation:

This is a contour plot of density. The more transparent the color, the low the density. Therefore, red, which is on the top of the color bar, is the most opaque color and represent the highest density, the next highest the grey and so on.

We can see there is a primitive disk like structure around two stars. Spiral shocks compress the disk, push the disk outwards and give it angular momentum.

contour.mov​

Since the angular frequency of the equatorial outflow is below the orbital angular frequency and we still see a circumbinary disk, it means that, it the outflow is induced by the in fall on a planet.

Future works:

  1. Include mass, momentum and angular momentum conservation of the sink particles so that we can study the orbital evolution.
  1. Add cooling. NK cooling preferred (D., Neufeld and M., Kaufman (1993)).

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