Abstract
There is intense interest about the family of emission features at 3.3, 3.4, 6.2, 7.7, 8.6, and 11.3 µm. These features are observed in many diverse types of astronomical objects (reviewed by Allamandola, 1984; Willner, 1984; Léger and d’Hendecourt, 1987; Mamandola, Tielens, and Barker, 1987). It has been postulated that these features may arise from aromatic hydrocarbons (Duley and Williams, 1981; Léger and Puget, 1984; Allamandola, Tielens and Barker, 1985). It has also been proposed by Sakata et al. (1984, 1987) that the emission features may arise from “quenched carbonaceous composite” (QCC), obtained from hydrocarbon plasma.
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Sakata, A., Wada, S., Onaka, T., Tokunaga, A.T. (1990). Quenced Carbonaceous Composite (QCC): Thermal Alteration of QCC and PAHs. In: Bussoletti, E., Vittone, A.A. (eds) Dusty Objects in the Universe. Astrophysics and Space Science Library, vol 165. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-0661-7_6
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DOI: https://doi.org/10.1007/978-94-009-0661-7_6
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