The 21 micron feature in the circumstellar envelopes around highly evolved stars

Details The 21 micron feature in the circumstellar envelopes around highly evolved stars The 21 micron feature in the circumstellar envelopes around highly evolved stars

Mar 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006pabei..24...43z&link_type=abstract

Progress in Astronomy (ISSN 1000-8349), Vol. 24, No. 1, p. 43 - 53 (2006)

Astronomy and Astrophysics

Astrophysics

2

Astrophysics, 21 Micron Feature, Review, Circumstellar Matter, Agb, Post-Agb, Stars

Scientific paper

The origin of the so-called 21 micron feature which is prominent in the infrared (IR) spectra of some carbon-rich proto-planetary nebular (PPNe) has been a mystery since its first detection in 1989. So far, this feature has been detected in 12 PPNe (and possibly in two planetary nebulae associated with Wolf-Rayet central stars). This feature has a similar intrinsic spectral shape and peaks at the same wavelength (20.1 μm) in all PPNe sources. These sources have quite uniform properties: they are mostly metal-poor, carbon-rich F and G supergiants with IR excesses and overabundant s-process elements. A large number of candidate carriers for this feature have been proposed in the past decade, including hydrogenated fullerenes, polycyclic aromatic hydrocarbon, hydrogenated amorphous carbon, diamonds, synthetic carbonaceous macromolecules, amides (especially urea), iron oxides (γ-Fe2O3, Fe3O4, FeO), SiS2, titanium carbide nanoclusters, doped SiC, and SiC core-SiO2 mantle particles. But none of them has been widely accepted. In this paper we review the observational characteristics of this feature and the proposed candidate materials.

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