Shaping planetary nebulae: is it different for [WR] stars? |
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| Authors: | Garrelt Mellema |
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| Institution: | (1) Stockholm Observatory, SE-133 36 Saltsjöbaden, Sweden |
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| Abstract: | This review discusses the physics of the formation of planetarynebulae around low mass WR stars, or WR] stars. It especially focuseson the differences which can be expected due to the differentcharacter of the fast winds from these WR] stars. Their fast windsare more massive and are highly H deficient and metal enrichedcompared to the winds of normal central stars of planetarynebulae. This is expected to lead to faster expansion velocities forthe nebulae and a longer momentum-driven phase in the evolution of thewind-driven bubble, leading to more turbulent nebulae. Theobservational evidence also shows that the process which produces theWR] stars is unlikely to influence the onset of aspherical mass loss,something which can be used as a test for models for aspherical massloss from AGB and post-AGB stars. Finally it is shown that thenebular characteristics rule out a very late He shell flash as theorigin of most WR] stars. |
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