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The morphology of dust emission in Planetary Nebulae and proto-Planetary Nebulae

Published online by Cambridge University Press:  25 May 2016

M. Meixner
M. Meixner*
Affiliation:
University of Illinois Department of Astronomy, 1002 W. Green St., Urbana, IL, 61801, USA

Abstract

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This review covers recent results from ground based mid-infrared (mid–IR; 8–25μm) imaging of thermal dust emission. The mid–IR images of proto–PNe show evidence for axially symmetric superwinds. In young PNe, the dust appears to be well mixed with the gas in the ionized gas regions. In carbon rich PNe and proto–PNe, the 11.3μm feature attributed to PAHs appears more spatially extended than “continuum” dust emission and the near–IR (1-3μm) excess appears spatially coincident with mid–IR dust emission. This review is not meant to cover the broader topic of dust in PNe and proto-PNe and we refer the reader to (Barlow 1993) for the most recent broad review.

Type
V. From AGB to Planetary Nebulae
Information
Symposium - International Astronomical Union , Volume 180: Planetary Nebulae , 1997 , pp. 325 - 331
Copyright
Copyright © Kluwer 1997 

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