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Shape, structure, and morphology in planetary nebulae

Published online by Cambridge University Press:  30 August 2012

Richard A. Shaw
Richard A. Shaw*
Affiliation:
National Optical Astronomy Observatory, Tucson, AZ 85719, USA email: shaw@noao.edu
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Abstract

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A revival over the past two decades in planetary nebula (PN) morphological studies springs from a combination of factors, including the advent of wide-area, high dynamic range detectors; the growing archives of high resolution images from the X-ray to the sub-mm; and the advent of sophisticated models of the co-evolution of PNe and their central stars. Yet the story of PN formation from their immediate precursors, the AGB stars, is not yet fully written. PN morphology continues to inspire, provide context for physical interpretation, and serve as an ultimate standard of comparison for many investigations in this area of astrophysics. After a brief review of the remarkable successes of PN morphology, I summarize how this tool has been employed over the last half-decade to advance our understanding of PNe.

Keywords

Planetary nebulae: generalISM: abundancesISM: jets and outflowsISM: molecules
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S283: Planetary Nebulae: An Eye to the Future , July 2011 , pp. 156 - 163
Copyright
Copyright © International Astronomical Union 2012

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