Stellar wind bubbles around WR and [WR] stars
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2 Stockholm Observatory, AlbaNova (SCFAB), Department of Astronomy, 106 91 Stockholm, Sweden e-mail: firstname.lastname@example.org
Corresponding author: G. Mellema, email@example.com
Accepted: 7 August 2002
We study the dynamics of stellar wind bubbles around hydrogen-deficient stars using numerical simulations with time- and ion dependent cooling. We consider two types of hydrogen-deficient stars, massive WR stars, producing Ring Nebulae, and low mass [WR] stars, producing Planetary Nebulae. We show that for the Planetary Nebulae, the different cooling properties of the hydrogen-deficient wind lead to a later transition from momentum- to energy-driven flow, which could explain the observed turbulence of these nebulae. We find that Ring Nebulae should all be energy-driven, and show how comparing the bubble's momentum and kinetic energy to the input wind momentum and kinetic energy, can give misleading information about the dynamics of the bubble.
Key words: planetary nebulae: general / ISM: bubbles / stars: Wolf–Rayet / stars: AGB and post–AGB / hydrodynamics
© ESO, 2002