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.
Fetch Pdf-File (sandin-IAU283.pdf, 77kB)