Crystalline silicates in planetary nebulae with [WC] central stars

LBFM Waters*, DA Beintema, AA Zijlstra, A de Koter, FJ Molster, J Bouwman, T de Jong, Stuart Pottasch, T de Graauw

*Corresponding author for this work

Research output: Contribution to journalLetterAcademicpeer-review

109 Citations (Scopus)

Abstract

We present ISO-SWS spectroscopy of the cool dusty envelopes surrounding two Planetary Nebulae with [WC] central stars, BD+30 3639 and He 2-113. The lambda <15 mu m region is dominated by a rising continuum with prominent emission from C-rich dust (PAHs), while the long wavelength part shows narrow solid state features from crystalline silicates. This demonstrates that the chemical composition of both stars changed very recently (less than 1000 years ago). The most likely explanation is a thermal pulse at the very end of the AGE or shortly after the AGE. The H-rich nature of the C-rich dust suggests that the change to C-rich chemistry did not remove all H. The present-day H-poor [WC] nature of the central star may be due to extensive mass loss and mixing following the late thermal pulse.

Original languageEnglish
Pages (from-to)L61-L64
Number of pages4
JournalAstronomy & astrophysics
Volume331
Issue number3
Publication statusPublished - Mar-1998

Keywords

  • Infrared : stars
  • stars : AGB and post-AGB
  • mass loss
  • planetary nebulae
  • dust
  • SHORT-WAVELENGTH SPECTROMETER
  • EMISSION FEATURES
  • SPECTRUM
  • BANDS
  • MINERALOGY
  • NUCLEI
  • DUST

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