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PG 1159-035
PG 1159-035 is the prototypical PG 1159 star after which the class of PG 1159 stars was named. It was discovered in the Palomar-Green survey of ultraviolet-excess stellar objects〔 and, like the other PG 1159 stars, is in transition between being the central star of a planetary nebula and being a white dwarf.〔(High-resolution ultraviolet spectroscopy of PG 1159-035 with HST and FUSE ), D. Jahn, T. Rauch, E. Reiff, K. Werner, and J. W. Kruk, ''Astronomy and Astrophysics'' 462, #1 (January 2007), pp. 281–292.〕
The luminosity of PG 1159-035 was observed to vary in 1979,〔(PG1159-035: A new, hot, non-DA pulsating degenerate ), J. T. McGraw, S. G. Starrfield, J. Liebert, and R. F. Green, pp. 377–381 in ''White Dwarfs and Variable Degenerate Stars'', IAU Colloquium #53, ed. H. M. van Horn and V. Weidemann, Rochester: University of Rochester Press, 1979.〕 and it was given the variable star designation ''GW Vir'' in 1985.〔(The 67th Name-List of Variable Stars ), P. N. Kholopov, N. N. Samus, E. V. Kazarovets, and N. B. Perova, ''Information Bulletin on Variable Stars'', #2681, March 8, 1985.〕 Variable PG 1159 stars may be called ''GW Vir'' stars, or the class may be split into ''DOV'' and ''PNNV'' stars.〔§1, (Detection of non-radial g-mode pulsations in the newly discovered PG 1159 star HE 1429-1209 ), T. Nagel and K. Werner, ''Astronomy and Astrophysics'' 426 (2004), pp. L45–L48.〕〔§1.1, (Mapping the Instability Domains of GW Vir Stars in the Effective Temperature-Surface Gravity Diagram ), Quirion, P.-O., Fontaine, G., Brassard, P., ''Astrophysical Journal Supplement Series'' 171 (2007), pp. 219–248.〕 The variability of PG 1139-035, like that of other GW Vir stars, arises from non-radial gravity wave pulsations within itself.〔(Asteroseismology of white dwarf stars ), D. E. Winget, ''Journal of Physics: Condensed Matter'' 10, #49 (December 14, 1998), pp. 11247–11261. DOI 10.1088/0953-8984/10/49/014.〕 Its light curve has been observed intensively by the (Whole Earth Telescope ) over a 264-hour period in March 1989, and over 100 of its vibrational modes have been found in the resulting vibrational spectrum, with periods ranging from 300 to 1,000 seconds.〔(Asteroseismology of the DOV star PG 1159-035 with the Whole Earth Telescope ), D. E. Winget, R. E. Nather, J. C. Clemens, J. Provencal, S. J. Kleinman, P. A. Bradley, M. A. Wood, C. F. Claver, M. L. Frueh, A. D. Grauer, B. P. Hine, C. J. Hansen, G. Fontaine, N. Achilleos, D. T. Wickramasinghe, T. M. K. Marar, S. Seetha, B. N. Ashoka, D. O'Donoghue, B. Warner, D. W. Kurtz, D. A. Buckley, J. Brickhill, G. Vauclair, N. Dolez, M. Chevreton, M. A. Barstow, J. E. Solheim, A. Kanaan, S. O. Kepler, G. W. Henry, and S. D. Kawaler, ''Astrophysical Journal'' 378 (September 1, 1991), pp. 326–346.〕
〔(The pulsation modes of the pre-white dwarf PG 1159-035 ), Costa, J. E. S.; Kepler, S. O.; Winget, D. E.; O'Brien, M. S.; Kawaler, S. D.; Costa, A. F. M.; Giovannini, O.; Kanaan, A.; Mukadam, A. S.; Mullally, F.; Nitta, A.; Provençal, J. L.; Shipman, H.; Wood, M. A.; Ahrens, T. J.; Grauer, A.; Kilic, M.; Bradley, P. A.; Sekiguchi, K.; Crowe, R.; Jiang, X. J.; Sullivan, D.; Sullivan, T.; Rosen, R.; Clemens, J. C.; Janulis, R.; O'Donoghue, D.; Ogloza, W.; Baran, A.; Silvotti, R.; Marinoni, S.; Vauclair, G.; Dolez, N.; Chevreton, M.; Dreizler, S.; Schuh, S.; Deetjen, J.; Nagel, T.; Solheim, J.-E.; Gonzalez Perez, J. M.; Ulla, A.; Barstow, M.; Burleigh, M.; Good, S.; Metcalfe, T. S.; Kim, S.-L.; Lee, H.; Sergeev, A.; Akan, M. C.; Çakırlı, Ö.; Paparo, M.; Viraghalmy, G.; Ashoka, B. N.; Handler, G.; Hürkal, Ö.; Johannessen, F.; Kleinman, S. J.; Kalytis, R.; Krzesinski, J.; Klumpe, E.; Larrison, J.; Lawrence, T.; Meištas, E.; Martinez, P.; Nather, R. E.; Fu, J.-N.; Pakštienė, E.; Rosen, R.; Romero-Colmenero, E.; Riddle, R.; Seetha, S.; Silvestri, N. M.; Vučković, M.; Warner, B.; Zola, S.; Althaus, L. G.; Córsico, A. H.; Montgomery, M. H., ''Astronomy and Astrophysics'' 477 (January 2, 2008), pp.627–640.〕
==References==
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