Bonding in hydrogenated hard carbon studied by optical spectroscopy

Dischler, B.; Bubenzer, A.; Koidl, P.

doi:10.1016/0038-1098(83)90936-5

Cited by 668 publications

(186 citation statements)

References 9 publications

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“…Two types of laboratory analogs from Mennella et al (1999) and Goto et al (2000) are shown for comparison. The vertical dotted lines indicate the asymmetric vibrational modes of C-H bonds in methyl (3.38 lm) and methylene groups (3.42 lm), and the symmetric vibrational mode of methylene groups (3.48 lm) (Dischler, Bubenzer, & Koidl 1983). nucleation and growth rates are very high there.…”

Section: Preserving Aliphatic Materialsmentioning

confidence: 99%

Spatially Resolved 3 Micron Spectroscopy of IRAS 22272+5435: Formation and Evolution of Aliphatic Hydrocarbon Dust in Proto–Planetary Nebulae

Goto

Gäessler

Hayano

et al. 2003

ApJ

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We present medium-resolution 3 lm spectroscopy of the carbon-rich proto-planetary nebula IRAS 22272+5435. Spectroscopy with the Subaru Telescope adaptive optics system revealed a spatial variation of hydrocarbon molecules and dust surrounding the star. The rovibrational bands of acetylene (C 2 H 2 ) and hydrogen cyanide (HCN) at 3.0 lm are evident in the central star spectra. The molecules are concentrated in the compact region near the center. The 3.3 and 3.4 lm emission of aromatic and aliphatic hydrocarbons is detected at 600-1300 AU from the central star. The separation of spatial distribution between gas and dust suggests that the small hydrocarbon molecules are indeed the source of solid material and that the gas left over from the grain formation is being observed near the central star. The intensity of aliphatic hydrocarbon emission relative to the aromatic hydrocarbon emission decreases with distance from the central star. The spectral variation is well matched to that of a laboratory analog thermally annealed with different temperatures. We suggest that either the thermal process after the formation of a grain or the variation in the temperature in the dust-forming region over time determines the chemical composition of the hydrocarbon dust around the proto-planetary nebula.

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Section: Preserving Aliphatic Materialsmentioning

confidence: 99%

Spatially Resolved 3 Micron Spectroscopy of IRAS 22272+5435: Formation and Evolution of Aliphatic Hydrocarbon Dust in Proto–Planetary Nebulae

Goto

Gäessler

Hayano

et al. 2003

ApJ

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“…The C-H vibrational absorption frequencies around 3000 cm Ϫ1 are given in Table II according to Dischler 21 and Dischler, Bubenzer, and Koidl. 22 Due to much overlap of the various peaks around 3000 cm Ϫ1 the deconvolution is rather complicated and some assumptions have to be made. One of them is the contribution of sp 3 CH 3 and sp 2 CH 2 bonds in the films.…”

Section: Film Analysismentioning

confidence: 99%

“…The hydrogen density decreases from about 9ϫ10 22 to 3ϫ10 22 cm Ϫ3 and is in rather good agreement with the ERDA/RBS values. In the second case one proportionality constant is assumed for all bonding types as, e.g., is assumed by Dischler and co-workers 22 and Jacob and Möller. 31 This results in an overall value of 2.7ϫ10 21 cm Ϫ2 for all bonding types.…”

Section: ͑2͒mentioning

confidence: 99%

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Optical and mechanical properties of plasma-beam-deposited amorphous hydrogenated carbon

Gielen

Kleuskens

Sanden

et al. 1996

Journal of Applied Physics

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Amorphous hydrogenated carbon films have been deposited on crystalline silicon and on glass from an expanding thermal plasma. Two deposition parameters have been varied: the electric current through the plasma source and the admixed acetylene flow. No energetic ion bombardment has been applied during deposition. Ex situ analysis of the films yields the infrared refractive index, hardness, Young's modulus, optical band gap, bonded hydrogen content, and the total hydrogen and mass density. The infrared refractive index describes the film properties independent of which plasma deposition parameter ͑arc current or acetylene flow͒ has been varied. The hardness, Young's modulus, sp 2 /sp 3 ratio, and mass density increase with increasing refractive index. The optical band gap and hydrogen content of the films decrease with increasing refractive index. It is demonstrated that plasma-beam-deposited diamondlike a-C:H has similar properties as material deposited with conventional plasma-enhanced chemical-vapor-depositions techniques under energetic ion bombardment.

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“…The structure of hydrogenated DLC can be described as a randbm network of covalently bonded carbon in hybridized tetragonal, (sp') and trigonal (sp') local coordination, with some of the bonds terminated by hydrogen [13]. Robertson [14,15] claimed that, in addition to the short-range order defined by carbon hybridization and hydrogen content, a substantial degree of medium-range order on about the 10 8, scale also exists in the films.…”

Section: Review Of Die Trhologymentioning

confidence: 99%