Of Wolf-Rayet central stars and common envelopes

Orsola De Marco*, Eric L. Sandquist, Mordecai M. Mac Low, Falk Herwig, Ronald E Taam

*Corresponding author for this work

Research output: Contribution to journalArticle

3 Scopus citations

Abstract

Although single star evolutionary calculations have recently succeeded in reproducing the composition of the hydrogen-deficient Wolf-Rayet (WR) central stars of planetary nebulae, it is clear from the latest infrared observations that a new perspective has to be adopted: the simultaneous presence of carbon- and oxygen-rich dust, while being a rare phenomenon for H-rich central stars, is found around the vast majority of cool WR central stars. De Marco & Soker (2002) proposed that the majority of WR central stars are the result of a merger with a low-mass companion during the asymptotic giant branch (AGB) phase. In this work, we partly test this speculative suggestion by 3-dimensional hydrodynamical models, which simulate the common envelope phase between 0.1 and 0.2M companions and an AGB star at the rst and tenth thermal pulse.

Original languageEnglish (US)
Pages (from-to)34-37
Number of pages4
JournalRevista Mexicana de Astronomia y Astrofisica: Serie de Conferencias
Volume15
StatePublished - Dec 1 2003

Keywords

  • Methods: numerical
  • Stars: AGB and post-AGB
  • Stars: evolution
  • Stellar dynamics

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

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