This page is a sub-set of the page developed by the group of Dr. Steve Kawaler at Iowa State University.

The animations below simulate the changing temperature distribution across the surface of nonradially pulsating white dwarf stars. These temperature variations cause the observed brightness variations. Each clip shows a single mode of pulsation. Modes are labeled with two integer indices. The first gives the number of lines on the surface which the temperature does not change. The second gives the number of such lines that pass through the poles. Note that the apparent rotation of the star is simply the pattern moving around star. In all these simulations the star itself is not rotating.

y10 Animated in MPEG
y10 Animated in QuickTime
y11 Animated in QuickTime

y20 Animated in QuickTime
y21 Animated in MPEG
y21 Animated in QuickTime

y22 Animated in QuickTime

y30 Animated in MPEG
y33 Animated in QuickTime Last Changed: 18 Jun 1996