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Morphology of Planetary Nebulae—Possible Effects of Rotation on Stellar Ejecta

Published online by Cambridge University Press:  26 May 2016

Sun Kwok
Sun Kwok*
Affiliation:
Department of Physics & Astronomy, University of Calgary, Calgary, Canada T2N 1N4

Abstract

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Planetary nebulae are formed as the result of the interaction between a slow stellar wind from the asymptotic giant branch progenitor and a later-developed fast outflow from the central star. Many of the morphological and kinematic properties of planetary nebulae have been successfully explained by this interacting stellar winds model. The observed diverse morphologies of planetary nebulae can also be understood if the slow wind is not spherically symmetric. However, new observational features such as collimated outflows and multi-polar lobes suggest that the fast wind may be non-isotropic and time variable. The possible roles of magnetic fields and rotation may play in the formation of these features are discussed.

Type
Session 4 Rotation and Stellar Evolution
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 473 - 478
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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