Laboratory and Theoretical Simulation of 3.4 μm Spectra of Hydrocarbons in Interstellar Sources

Duley, W. W.; Grishko, Victor I.; Kenel, J.; Lee-Dadswell, G. R.; Scott, Andrew D.

doi:10.1086/430084

Cited by 18 publications

(31 citation statements)

References 36 publications

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“…The bonds with neighboring carbon atoms that are freed after the removal of the hydrogen atom form new bonds, which gradually form a closed ring: the structure of the dust grains makes a transition from an aliphatic to an aromatic state [27,28]. Laboratory studies of this process are presented in [26][27][28]48], and theoretical computations of its rate are described in [49,50].…”

Section: Interaction With Radiationmentioning

confidence: 99%

Restructuring and destruction of hydrocarbon dust in the interstellar medium

Murga¹,

Khoperskov²,

Wiebe³

2016

Astron. Rep.

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A model of key processes influencing the evolution of a hydrocarbon grain of an arbitrary size under astrophysical conditions corresponding to ionized hydrogen regions (HII regions) and supernova remnants is presented. The considered processes include aromatization and photodestruction, sputtering by electrons and ions, and shattering due to collisions between grains. The model can be used to simulate the grain size distribution and the aromatization degree during the evolution of HII regions and supernova remnants for a specified radiation field, relative velocity of gas and dust, etc. The contribution of various processes to the evolution of hydrocarbon dust grains for parameters typical for the interstellar medium of our Galaxy is pre-

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Section: Interaction With Radiationmentioning

confidence: 99%

Restructuring and destruction of hydrocarbon dust in the interstellar medium

Murga¹,

Khoperskov²,

Wiebe³

2016

Astron. Rep.

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“…Because it falls squarely in the region associated with the aliphatic CÀH stretch, it is commonly assigned to aliphatic CÀH stretching motions. The aliphatic CÀH stretching vibrations can arise from aliphatic side groups on PAHs (de Muizon et al 1990;Joblin et al 1996;Duley et al 2005;Sloan et al 1997) or from PAHs containing excess H atoms (H n -PAHs; Schutte et al 1993;Bernstein et al 1996). The extent of each one's contribution to the emission depends on the conditions in the local environment.…”

Section: Introductionmentioning

confidence: 99%

The Energetics for Hydrogen Addition to Naphthalene Cations

Ricca

Bakes

Bauschlicher

2007

ApJ

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Energetics of H-addition reactions to the naphthalene cation are determined using computational chemistry techniques. While most of the reactions have little to no barrier, the shape of the potential energy surfaces favors the formation of the product with the added hydrogen atoms being on adjacent carbons. Thus, while many products will be formed, one expects that the product in which all the hydrogen atoms are added to the same or adjacent rings will be favored over a random distribution of added hydrogen atoms. This has implications on the species that will be formed when polycyclic aromatic hydrocarbons (PAHs) are photolyzed in ices in the interstellar medium (ISM ). Barrierless reactions are consistent with the view that PAHs with extra hydrogens contribute to the 3.4 m band.

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“…The changes in the shape and relative intensity of these bands in the different environments where they are observed reflect the dependence of the carrier composition on the ambient conditions. Comparison of observational and laboratory spectra shows that hydrocarbons in the diffuse ISM (DISM) contain more methyl groups than in dark clouds whereas methylene groups are always present [30].…”

Section: -P6mentioning

confidence: 99%

Interstellar dust within the life cycle of the interstellar medium

Demyk

2011

EPJ Web of Conferences

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Abstract. Cosmic dust is omnipresent in the Universe. Its presence influences the evolution of the astronomical objects which in turn modify its physical and chemical properties. The nature of cosmic dust, its intimate coupling with its environment, constitute a rich field of research based on observations, modelling and experimental work. This review presents the observations of the different components of interstellar dust and discusses their evolution during the life cycle of the interstellar medium.

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Laboratory and Theoretical Simulation of 3.4 μm Spectra of Hydrocarbons in Interstellar Sources

Cited by 18 publications

References 36 publications

Restructuring and destruction of hydrocarbon dust in the interstellar medium

Restructuring and destruction of hydrocarbon dust in the interstellar medium

The Energetics for Hydrogen Addition to Naphthalene Cations

Interstellar dust within the life cycle of the interstellar medium

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