Theoretical modeling of the infrared fluorescence from interstellar polycyclic aromatic hydrocarbons

Details Theoretical modeling of the infrared fluorescence from interstellar polycyclic aromatic hydrocarbons Theoretical modeling of the infrared fluorescence from interstellar polycyclic aromatic hydrocarbons

Sep 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993apj...415..397s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 415, no. 1, p. 397-414.

Astronomy and Astrophysics

Astronomy

184

Aromatic Compounds, Cyclic Hydrocarbons, Fluorescence, Infrared Spectra, Interstellar Matter, Interstellar Radiation, Infrared Astronomy Satellite, Molecular Spectra, Size Distribution

Scientific paper

We have modeled the family of interstellar IR emission bands at 3.3, 6.2, 7.7, 8.6, 11.3, and 12.7 microns by calculating the fluorescence from a size distribution of interstellar polycyclic aromatic hydrocarbons (PAHs) embedded in the radiation field of a hot star. It is found that the various emission bands are dominated by distinctly different PAHs, from molecules with much less than about 80 C atoms for the 3.3 micron feature, to molecules with 10 exp 2-10 exp 5 C atoms for the emission in the IRAS 12 and 25 micron bands. We quantitatively describe the influence on the emergent spectrum of various PAH properties such as the molecular structure, the amount of dehydrogenation, the intrinsic strength of the IR active modes, and the size distribution. Comparing our model results to the emission spectrum from the Orion Bar region, we conclude that interstellar PAHs are likely fully, or almost fully, hydrogenated. Moreover, it is found that the intrinsic strengths of the 6.2 and 7.7 micron C-C stretching modes, and the 8.6 micron C-H in-plane bending mode are 2-6 times larger than measured for neutral PAHs in the laboratory.

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