The role of heat conduction to the formation of [WC]-type Planetary Nebulae

C. Sandin, M. Steffen, R. Jacob, D. Schönberner, U. Rühling, W.-R. Hamann, H. Todt

X-ray observations of young Planetary Nebulae (PNe) have revealed diffuse emission in extended regions, around both H-rich and H-deficient central stars. In order to also reproduce physical properties of H-deficient objects, we have, at first, extended our time-dependent radiation-hydrodynamic models with heat conduction for such conditions. Here we present some of the important physical concepts, which determine how and when a hot wind-blown bubble forms. In this study we have had to consider the, largely unknown, evolution of the CSPN, the slow (AGB) wind, the fast hot-CSPN wind, and the chemical composition. The main conclusion of our work is that heat conduction is needed to explain X-ray properties of wind-blown bubbles also in H-deficient objects.

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