PG 1159-035

PG 1159-035

Starbox begin
name= [ PG 1159-035]
Starbox observe
epoch=J2000.0 (ICRS)
ra=RA|12|01|46.1 [ The Palomar-Green catalog of ultraviolet-excess stellar objects] , R. F. Green, M. Schmidt, and J. Liebert, "Astrophysical Journal Supplement" 61 (June 1986), pp. 305–352. CDS ID [ II/207] .]
appmag_v=14.9SIMBAD, accessed June 11, 2007.]
Starbox catalog
names=GW Vir, GW Virginis, 2E 2572, WD 1159-034

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.]


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