The UV (IUE) spectrum of the planetary nebula PC 11 (HD 149427)

M Parthasarathy*, P Garcia-Lario, [No Value] Pottasch, D de Martino, R Surendiranath

*Corresponding author for this work

Research output: Contribution to journalArticleAcademicpeer-review

6 Citations (Scopus)

Abstract

The UV spectrum of PC 11 is found to show variations in the strength of the O III] 1666 Angstrom, N III] 1750 Angstrom and C III] 1909 Angstrom emission lines. The detection of continuum emission in the wavelength interval 2650 Angstrom to 3200 Angstrom indicates that the central star of PC 11 has an early F-type dwarf companion. The very low level of UV continuum in the wavelength interval 1150 Angstrom to 1900 Angstrom and the non-detection of the central star in the UV images recently taken with I-IST suggest that the hot whitedwarf or sub-dwarf like central star may be obscured by a dusty disk. The variations in the UV emission lines observed during the period 1987 to 1994 may be the consequence of variable emission coming from high-velocity jet-like emission visible in optical images also taken with HST in the light of [O III]. Based on our UV observations, we confirm our identification of PC 11 as a planetary nebula with a close binary central star. Adopting the absolute magnitude of a F0V companion yields a distance of 485 pc to PC 11. If we assume a typical expansion velocity of 12.5 km s(-1) and considering the observed angular diameter of the nebula (4.1 "), we find the age of PC 11 to be 376 years. The AGE phase of evolution of the central star seems to have been terminated only recently.

Original languageEnglish
Pages (from-to)720-724
Number of pages5
JournalAstronomy & astrophysics
Volume355
Issue number2
Publication statusPublished - Mar-2000

Keywords

  • ISM : planetary nebulae : individual
  • ultraviolet : stars
  • stars : binaries : close
  • stars : evolution
  • stars : emission-line, Be
  • stars : AGB and post-AGB
  • STARS

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