AAS 199th meeting, Washington, DC, January 2002
Session 93. Data Analysis Challenges in Solar Stellar Astrophysics
Display, Wednesday, January 9, 2002, 9:20am-6:30pm, Exhibit Hall

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[93.03] Nonlinear Time Series Analysis of White Dwarf Light Curves

N. Jevtic (Physics Dept., U. Connecticut), S. Zelechoski (U. Connecticut 2001 REU Program, UCSD), H. Feldman (U. Connecticut 2001 REU Program, U. California, Berkeley), C. Peterson, J. Schweitzer (Physics Dept., U. Connecticut)

We use nonlinear time series analysis methods to examine the light intensity curves of white dwarf PG1351+489 obtained by the Whole Earth Telescope (WET). Though these methods were originally introduced to study chaotic systems, when a clear signature of determinism is found for the process generating an observable and it couples the active degrees of freedom of the system, then the notion of phase space provides a framework for exploring the system dynamics of nonlinear systems in general. With a pronounced single frequency, its harmonics and other frequencies of lower amplitude on a broadband background, the PG1351 light curve lends itself to the use of time delay coordinates. Our phase space reconstruction yields a triangular, toroidal three-dimensional shape. This differs from earlier results of a circular toroidal representation. We find a morphological similarity to a magnetic dynamo model developed for fast rotators that yields a union of both results: the circular phase space structure for the ascending portion of the cycle, and the triangular structure for the declining portion. The rise and fall of the dynamo cycle yield both different phase space representations and different correlation dimensions. Since PG1351 is known to have no significant fields, these results may stimulate the observation of light curves of known magnetic white dwarfs for comparison.

Using other data obtained by the WET, we compare the phase space reconstruction of DB white dwarf PG1351 with that of GD 358 which has a more complex power spectrum. We also compare these results with those for PG1159. There is some general similarity between the results of the phase space reconstruction for the DB white dwarfs. As expected, the difference between the results for the DB white dwarfs and PG1159 is great.

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