Hydrocarbon emission features in the IR spectra of warm supergiants

Details Hydrocarbon emission features in the IR spectra of warm supergiants Hydrocarbon emission features in the IR spectra of warm supergiants

Dec 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990apj...365l..23b&link_type=abstract

Astrophysical Journal, Part 2 - Letters (ISSN 0004-637X), vol. 365, Dec. 10, 1990, p. L23-L26.

Astronomy and Astrophysics

Astrophysics

88

Cyclic Hydrocarbons, Infrared Spectra, Interstellar Matter, Stellar Spectra, Supergiant Stars, Aromatic Compounds, Asymptotic Giant Branch Stars, Emission Spectra, Planetary Nebulae

Scientific paper

Observations in the 3-13 micron range are presented for two objects possessing the unidentified 21-micron feature, IRAS 22272 and IRAS 07134, which were obtained in the course of search for circumstellar aromatic hydrocarbon (PAH) emission bands. The 3.3 and 6.2 micron bands are attributed to circumstellar PAH molecules, and the 6-9 micron plateau and the 12- and 6.9-micron lines are attributed to larger, aromatic hydrocarbon clusters. These are the coolest stars known to exhibit the IR emission bands. The 21-micron feature is conjectured to also originate in a carbonaceous carrier.

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