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Morphological Structures of Planetary Nebulae

Published online by Cambridge University Press:  02 January 2013

Sun Kwok
Sun Kwok
Affiliation:
Faculty of Science, The University of Hong Kong, Hong Kong, China. Email: sunkwok@hku.hk
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Abstract

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Since various structural components of planetary nebulae (PN) manifest themselves differently, a combination of optical, infrared, submillimetre and radio techniques is needed to derive a complete picture of planetary nebulae. The effects of projection can also make derivation of the true 3-D structure difficult. Using a number of examples, we show that bipolar and multipolar nebulae are much more common than usually inferred from morphological classifications of apparent structures of planetary nebulae. We put forward a new hypothesis that the bipolar and multipolar lobes of PN are not regions of high-density ejected matter, but the result of ionization and illumination. The visible bright regions are in fact volumes of low density (cleared by high-velocity outflows), through which UV photons are being channelled. We suggest that multipolar nebulae with similar lobe sizes are not caused by simultaneous ejection of matter in several directions, but by leakage of UV photons in those directions.

Keywords

planetary nebulae: generalstars: AGB and post-AGBstars: mass loss

Information

Type
Research Article
Information
Publications of the Astronomical Society of Australia , Volume 27 , Issue 2 , 2010 , pp. 174 - 179
Copyright
Copyright © Astronomical Society of Australia 2010

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