Of Wolf-Rayet Central Stars and Common Envelopes

Details Of Wolf-Rayet Central Stars and Common Envelopes Of Wolf-Rayet Central Stars and Common Envelopes

Jan 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003rmxac..15...34d&link_type=abstract

Winds, Bubbles, and Explosions: a conference to honor John Dyson, Pátzcuaro, Michoacán, México, September 9-13, 2002 (Eds. S. J.

Astronomy and Astrophysics

Astronomy

5

Methods: Numerical, Stars: Agb And Post-Agb, Stars: Evolution, Stellar Dynamics

Scientific paper

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 0.2 M[ sun ]companions and an AGB star at the first and tenth thermal pulse.

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