RHO is density, U is horizontal velocity, and V is vertical velocity. For more frames, click here.
Here's a frame from a Lagrangian (SPH: smooth-particle hydrodynamics) simulation of a neutron star encountering a close binary, colliding with one component and severely disrupting (and ejecting) the other. Collisions such as this may be responsible for the production of isolated millisecond pulsars in globular clusters. The thick disk formed around the neutron star when it is ``smothered'' by the binary component it hits may conceivably spin the neutron star up to breakup speeds in a very short period of time.
Here's a movie.
This simulation was carried out by Drexel undergraduate William Palmer, using the Cray Y-MP at the Pittsburgh Supercomputer Center, as part of his senior project. Here are some more runs:
