Here are some plots of the mean value of omega (W_mean) as a function of cylindrical R and Z at four separate times during our long, "fast" evolution. Below this composite image is a link to the relevant movie from which the images were drawn.

t/P = 15.0	t/P = 18.3	t/P = 21.7	t/P = 23.1
Frames taken from the accompanying 3.8 MB Quicktime Movie

The standard rainbow color scheme is such that "red" identifies material that is spinning faster than W_frame while "blue" identifies material that is spinning more slowly than W_frame. Note that material that is moving at the frame frequency has been colored "black". This allows you to identify something akin to the corotation radius inside the star.

Here are some conclusions I draw from these images, and their accompanying movie:

• The star becomes more spherical with time.

• The star is being divided into two fairly distinct kinematical regions:
  1. An outer, relatively thin "surface" shell;
  2. A relatively large, central volume (mostly blue in the images shown above).

• Overall, the surface shell is moving faster than the mean and the central volume is moving more slowly than the mean.

• As you move in latitude from the "north" pole toward the equator, the surface shell exhibits a considerable amount of differential rotation. Specifically, the polar regions are spinning faster than the equatorial region.

• Until quite late in the evolution, the central volume is spinning fairly uniformly.

Finally, in order for the star to become more spherical with time, there must be a net redistribution of angular momentum "inward." It looks like this happens preferentially within the surface shell, with higher specific angular momentum material being transported to the polar region(s). In the equatorial plane, for example, there appears to be very little redistribution of angular momentum toward the axis of rotation; all the redistribution is occurring in the surface shell.