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Convective driving, the mechanism originally proposed by Brickhill (1991,1983) for pulsating white dwarf stars, has gained general acceptance as thegeneric linear instability mechanism in DAV and DBV white dwarfs. This physicalmechanism naturally leads to a nonlinear formulation, reproducing the observedlight curves of many pulsating white dwarfs. This numerical model can alsoprovide information on the average depth of a star's convection zone and theinclination angle of its pulsation axis. In this paper, we give two sets ofresults of nonlinear light curve fits to data on the DBV GD 358. Our first fitis based on data gathered in 2006 by the Whole Earth Telescope (WET); this dataset was multiperiodic, containing at least 12 individual modes. Our second fitutilizes data obtained in 1996, when GD 358 underwent a dramatic change inexcited frequencies accompanied by a rapid increase in fractional amplitude;during this event it was essentially monoperiodic. We argue that GD 358'sconvection zone was much thinner in 1996 than in 2006, and we interpret this asa result of a short-lived increase in its surface temperature. In addition, wefind strong evidence of oblique pulsation using two sets of evenly splittriplets in the 2006 data. This marks the first time that oblique pulsation hasbeen identified in a variable white dwarf star.

Evidence for Temperature Change and Oblique Pulsation from Light Curve Fits of the Pulsating White Dwarf GD 358