On the inorganic carriers of the 21 micron emission feature in post-AGB stars

Details On the inorganic carriers of the 21 micron emission feature in post-AGB stars On the inorganic carriers of the 21 micron emission feature in post-AGB stars

Oct 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008iaus..251..215z&link_type=abstract

Organic Matter in Space, Proceedings of the International Astronomical Union, IAU Symposium, Volume 251, p. 215-216

Astronomy and Astrophysics

Astronomy

Infrared: Stars, (Stars:) Circumstellar Matter, Stars: Agb And Post-Agb

Scientific paper

The mysterious 21 μm emission feature seen in only 12 C-rich proto-planetary nebulae (PPNe) remains unidentified since its discovery in 1989. Over a dozen materials have been suggested as the carrier candidates while none of them has received general acceptance. We investigate the inorganic carrier candidates by applying the observational constraints of the feature strength and associated features. It is found that: (1) three candidates, TiC clusters, fullerenes with Ti impurity atoms, and SiS2, are not abundant enough to account for the emission power of the 21 μm band, (2) five candidates, doped-SiC, SiO2-mantled SiC dust, carbon and silicon mixtures, Fe2O3, and Fe3O4, all show associated features which are either not detected in the 21 μm sources or detected but with a much lower strength, and (3) FeO, which satisfies the abundance constraints, does not display any associated features which are not seen in the 21 μm sources. Moreover, FeO is more likely to survive in the C-rich environment than Fe2O3 and Fe3O4. Thus FeO seems to be the most plausible one among the inorganic carrier candidates.

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