Abstract
The mid-infrared interstellar emission spectrum with features at 3050, 1610, 1300, 1150, and 885 cm-1 (3.28, 6.2, 7.7, 8.7 and 11.3 microns) is discussed in terms of the Polycyclic Aromatic Hydrocarbon (PAH) hypothesis. This hypothesis is based on the suggestive, but inconclusive comparison between the interstellar emission spectrum with the infrared absorption and Raman spectra of a few PAHs. The fundamental vibrations of PAHs and PAH-like species which determine the IR and Raman properties are discussed. Interstellar IR band emission is due to relaxation from highly vibrationally excited PAHs which have been excited by ultraviolet photons. The excitation/emission process is described in general and the IR fluorescence from one PAH, chrysene, is traced in detail. Generally, there is sufficient energy to populate several vibrational levels in each mode. Molecular vibrational potentials are anharmonic and emission from these higher levels will fall at lower frequencies and produce weak features to the red of the stronger fundamentals. This process is also described and can account for some spectroscopic details of the interstellar emission spectra previously unexplained. Analysis of the interstellar spectrum shows that PAHs containing between 20 and 30 carbon atoms are responsible for the emission.
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Allamandola, L.J., Tielens, A.G.G.M., Barker, J.R. (1987). Infrared Absorption and Emission Characteristics of Interstellar PAHs. In: Hollenbach, D.J., Thronson, H.A. (eds) Interstellar Processes. Astrophysics and Space Science Library, vol 134. Springer, Dordrecht. https://doi.org/10.1007/978-94-009-3861-8_17
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DOI: https://doi.org/10.1007/978-94-009-3861-8_17
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