PG 1159-035

PG 1159-035
Observation data
Epoch J2000.0      Equinox J2000.0 (ICRS)
Constellation Virgo
Right ascension 12h 01m 46.1s[1]
Declination −03° 45′ 39″[1]
Apparent magnitude (V) 14.9[2]
Astrometry
Distance1,400 ± 100 ly
(440 ± 40[3] pc)
Details
Mass0.59 ± 0.01[3] M☉
Radius0.0254 ± 0.005[3] R☉
Luminosity (bolometric)200[3] L☉
Surface gravity (log g)7.38 ± 0.1[3] cgs
Temperature136,000[3] K
Other designations
GW Vir, GW Virginis, 2E 2572, WD 1159-034
Database references
SIMBADdata

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[1] and, like the other PG 1159 stars, is in transition between being the central star of a planetary nebula and being a white dwarf.[4]

The luminosity of PG 1159-035 was observed to vary in 1979,[5] and it was given the variable star designation GW Vir in 1985.[6] Variable PG 1159 stars may be called GW Vir stars, or the class may be split into DOV and PNNV stars.[7][8] The variability of PG 1139-035, like that of other GW Vir stars, arises from non-radial gravity wave pulsations within itself.[9] 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.[10] [11]

References

  1. 1 2 3 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.
  2. ↑ SIMBAD, accessed June 11, 2007.
  3. 1 2 3 4 5 6 Table 2, Precision asteroseismology of pulsating PG 1159 stars, Steven D. Kawaler and Paul A. Bradley, Astrophysical Journal, Part 1 427, #1 (May 1994), pp. 415–428, doi:10.1086/174152, Bibcode: 1994ApJ...427..415K.
  4. ↑ 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.
  5. ↑ 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.
  6. ↑ 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.
  7. ↑ §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.
  8. ↑ §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.
  9. ↑ 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.
  10. ↑ 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.
  11. ↑ 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.
This article is issued from Wikipedia - version of the 12/2/2015. The text is available under the Creative Commons Attribution/Share Alike but additional terms may apply for the media files.