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The role of heat conduction to the formation of [WC]-type planetary nebulae
Published online by Cambridge University Press: 30 August 2012
Abstract
X-ray observations of young Planetary Nebulæ (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.
- Type
- Contributed Papers
- Information
- Proceedings of the International Astronomical Union , Volume 7 , Symposium S283: Planetary Nebulae: An Eye to the Future , July 2011 , pp. 494 - 495
- Copyright
- Copyright © International Astronomical Union 2012
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