Stellar wind bubbles around WR and [WR] stars

Abstract

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.

9 pages, 3 figures, to be published in A&A

References in corpus (2)

• Internal mixing and surface abundance of [WC]-CSPN
• Self-similar evolution of wind-blown bubbles with mass loading by hydrodynamic ablation

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