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Asteroseismology of the DOV star PG 1159 - 035 with the Whole Earth Telescope
Winget, D. E.; Nather, R. E.; Clemens, J. C.; Provencal, J.; Kleinman, S. J.; Bradley, P. A.; Wood, M. A.; Claver, C. F.; Frueh, M. L.; Grauer, A. D.; Hine, B. P.; Hansen, C. J.; Fontaine, G.; Achilleos, N.; Wickramasinghe, D. T.; Marar, T. M. K.; Seetha, S.; Ashoka, B. N.; O'Donoghue, D.; Warner, B.; Kurtz, D. W.; Buckley, D. A.; Brickhill, J.; Vauclair, G.; Dolez, N.; Chevreton, M.; Barstow, M. A.; Solheim, J. E.; Kanaan, A.; Kepler, S. O.; Henry, G. W.; Kawaler, S. D.
AA(Texas, University; McDonald Observatory, Austin), AB(Texas, University; McDonald Observatory, Austin), AC(Texas, University; McDonald Observatory, Austin), AD(Texas, University; McDonald Observatory, Austin), AE(Texas, University; McDonald Observatory, Austin), AF(Texas, University; McDonald Observatory, Austin), AG(Texas, University; McDonald Observatory, Austin), AH(Texas, University; McDonald Observatory, Austin), AI(Texas, University; McDonald Observatory, Austin), AJ(Arkansas, University, Little Rock)
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 378, Sept. 1, 1991, p. 326-346. Research supported by NSERC, CNRS, SERC, et al. (ApJ Homepage)
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NASA/STI Keywords:
Power Spectra, Pulsars, Stellar Luminosity, White Dwarf Stars, Data Acquisition, Fine Structure, Light Curve, Seismology, Telescopes
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Results are reported from 264.1 hr of nearly continuous time-series photometry on the pulsating prewhite dwarf star (DPV) PG 1159 - 035. The power spectrum of the data set is completely resolved into 125 individual frequencies; 101 of them are identified with specific quantized pulsation modes, and the rest are completely consistent with such modal assignment. It is argued that the luminosity variations are certainly the result of g-mode pulsations. Although the amplitudes of some of the peaks exhibit significant variations on the time scales of a year or so, the underlying frequency structure of the pulsations is stable over much longer intervals. The existing linear theory is invoked to determine, or strongly constrain, many of the fundamental physical parameters describing this star. Its mass is found to be 0.586 solar mass, is rotation period 1.38 days, its magnetic field less than 6000 G, its pulsation and rotation axes to be aligned, and its outer layers to be compositionally stratified.

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