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On the morphology and internal kinematics of PNe

Published online by Cambridge University Press:  25 May 2016

A. Manchado
A. Manchado*
Affiliation:
Instituto de Astrofísica de Canarias E-38200 La Laguna (Tenerife) Spain

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The study of the morphology of planetary nebula (PN) is fundamental for addressing several questions in the context of stellar evolution. An AGB star can loose most of its mass due to strong stellar winds. Kwok et al. (1978) proposed that the interaction of a low-density fast wind with a high-density slow wind, will form the PN. This model can account for the round observed PNe with a great degree of symmetry. However as we will see later, round PNe are not the most common ones. Therefore a mechanism for causing asymmetry has to be invoked. Several processes have been proposed by different authors.

Type
IV. Envelopes
Information
Symposium - International Astronomical Union , Volume 180: Planetary Nebulae , 1997 , pp. 184 - 189
Copyright
Copyright © Kluwer 1997 

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