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Dust in planetary nebulae

Published online by Cambridge University Press:  08 August 2017

G. C. Sloan Open the ORCID record for G. C. Sloan [Opens in a new window]
G. C. Sloan*
Affiliation:
Space Telescope Science Institute, 3700 San Martin Dr., Baltimore, MD 21218, USA Department of Physics and Astronomy, University of North Carolina, Chapel Hill, NC 27599-3255, USA Cornell Center for Astrophysics and Planetary Science, Cornell University, Ithaca, NY 14850-6801, USA
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Abstract

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Infrared spectra from the Spitzer Space Telescope trace the evolution of carbon-rich dust from the asymptotic giant branch (AGB) to young planetary nebulae (PNe). On the AGB, amorphous carbon dominates the dust, but SiC and MgS also appear. In more evolved systems with warmer central stars, the spectra reveal the unidentified 21 μm feature, features from aliphatic hydrocarbons, and spectra from polycyclic aromatic hydrocarbons (PAHs), often with shifted feature positions indicative of the presence of aliphatics. More evolved systems with hot central stars show more typical PAH spectra, along with fullerenes and/or an emission feature known as the big-11 feature at ~11 μm. This features arises from a combination of SiC and PAHs, and it is usually accompanied by a shoulder at 18 μm, which while unidentified might be from cool silicate grains. The strong emission from MgS and SiC in young PNe probably arises from coatings on carbonaceous grains.

Keywords

stars: AGB and post-AGBplanetary nebulae: generaldust
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S323: Planetary Nebulae: Multi-Wavelength Probes of Stellar and Galactic Evolution , October 2016 , pp. 121 - 127
Copyright
Copyright © International Astronomical Union 2017 

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