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ISO Spectra of Planetary Nebulae

Published online by Cambridge University Press:  26 May 2016

Kevin Volk  and
Sun Kwok
Kevin Volk
Affiliation:
Dept. of Physics and Astronomy, University of Calgary, Calgary, Canada T2N 1N4
Sun Kwok
Affiliation:
Dept. of Physics and Astronomy, University of Calgary, Calgary, Canada T2N 1N4

Extract

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It has been well known since the IRAS mission that dust emission represents a significant fraction of the energy output from PNe (Zhang & Kwok 1991). Although the dust component in PNe was long thought to be due to the remnants of the envelopes of AGB stars (Kwok 1982), we now know that dust in PNe has a much richer chemical composition. In addition to amorphous silicates and SiC features commonly seen in AGB stars, PNe have been found to have strong aromatic infrared features (Russell et al. 1977), crystalline silicate features (Waters et al. 1997), and an unidentified emission feature at 30 μm (Forrest et al. 1981). In this paper, we show the ISO spectra of a number of PNe illustrating the diverse dust chemistry in PNe.

Type
Part V: Dust and Molecules in Planetary Nebulae
Information
Symposium - International Astronomical Union , Volume 209: Planetary Nebulae: Their Evolution and Role in the Universe , 2003 , pp. 303 - 304
Copyright
Copyright © Astronomical Society of the Pacific 2003 

References

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