THE STRUCTURE, ORIGIN, AND EVOLUTION OF INTERSTELLAR HYDROCARBON GRAINS

Many materials have been considered for the carrier of the hydrocarbon absorption bands observed in the diffuse interstellar medium (ISM). In order to refine the model for ISM hydrocarbon grains, we analyze the observed aromatic (3.28, 6.2 mu m) and aliphatic (3.4 mu m) hydrocarbon absorption featur...

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Bibliographic Details
Published in:The Astrophysical journal 2013-06, Vol.770 (1), p.1-13
Main Authors: CHIAR, J E, TIELENS, A G G M, Adamson, A J, Ricca, A
Format: Article
Language:English
Subjects:
ABSORPTION
Aliphatic compounds
ASTROPHYSICS
ASTROPHYSICS, COSMOLOGY AND ASTRONOMY
CARBON
Diffusion
Dust
Evolution
Grains
HYDROCARBONS
HYDROGENATION
Interstellar
PHASE DIAGRAMS
SPECTRA
STAR EVOLUTION
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Summary:Many materials have been considered for the carrier of the hydrocarbon absorption bands observed in the diffuse interstellar medium (ISM). In order to refine the model for ISM hydrocarbon grains, we analyze the observed aromatic (3.28, 6.2 mu m) and aliphatic (3.4 mu m) hydrocarbon absorption features in the diffuse ISM along the line of sight toward the Galactic center Quintuplet Cluster. Observationally, sp super(2) bonds can be measured in astronomical spectra using the 6.2 mu m CC aromatic stretch feature, whereas the 3.4 mu m aliphatic feature can be used to quantify the fraction of sp super(3) bonds. The fractional abundance of these components allows us to place the Galactic diffuse ISM hydrocarbons on a ternary phase diagram. We conclude that the Galactic hydrocarbon dust has, on average, a low H/C ratio and sp super(3) content and is highly aromatic. We have placed the results of our analysis within the context of the evolution of carbon dust in the ISM. We argue that interstellar carbon dust consists of a large core of aromatic carbon surrounded by a thin mantle of hydrogenated amorphous carbon (a-C:H), a structure that is a natural consequence of the processing of stardust grains in the ISM.
ISSN:0004-637X
1538-4357
DOI:10.1088/0004-637X/770/1/78