3D Simulation of the accretion disk

Use the previous simulation of RLOF to supply boundary conditions for an incoming tidal stream.

Numerical grid is now centered on the accreting star, providing consistently high resolution throughout the disk.

The simulation is initialized with an isothermal alpha-disk model extending out to large radii. As the evolution begins, tidal forces quickly strip the outer disk down to a radius of roughly 1/2 the size of the Roche lobe.

Click here for a closer view of the inner regions of the disk. Note that the inner region is "frozen" for the first half of the simulation in order to evolve with a larger timestep (which is otherwise restricted by the high orbital velocities at small radii).


Density in the equatorial plane

Nearly Keplerian flow - slightly off center

Disk is truncated at 0.22a, roughly half the size of the Roche lobe radius, and twice the size of the circularization radius

The disk rim is flared as a result of stream impact.

Mass is accreting all the way through the disk