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| Naji, M. |
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| Motta, Antonella |
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| Aletan, Dirar |
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| Mohamed, Tarek |
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| Ertürk, Emre |
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| Taccardi, Nicola |
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| Kononenko, Denys |
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| Petrov, R. H. | Madrid |
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| Alshaaer, Mazen | Brussels |
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| Bih, L. |
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| Casati, R. |
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| Muller, Hermance |
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| Kočí, Jan | Prague |
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| Šuljagić, Marija |
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| Kalteremidou, Kalliopi-Artemi | Brussels |
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| Azam, Siraj |
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| Ospanova, Alyiya |
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| Blanpain, Bart |
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| Ali, M. A. |
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| Popa, V. |
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| Rančić, M. |
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| Ollier, Nadège |
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| Azevedo, Nuno Monteiro |
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| Landes, Michael |
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| Rignanese, Gian-Marco |
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Jones, Anthony
in Cooperation with on an Cooperation-Score of 37%
Topics
Publications (20/20 displayed)
- 2021BEDE: Bayesian estimates of dust evolution for nearby galaxiescitations
- 2015Amorphous Hydrocarbon Optical Properties
- 2015Dust variations in the diffuse interstellar medium: constraints on Milky Way dust from Planck-HFI observationscitations
- 2014A hidden reservoir of Fe/FeS in interstellar silicates?citations
- 2013The Circle of Dust: From Nanoparticles to Macromolecules and Beyond
- 2013Heteroatom-doped hydrogenated amorphous carbons, a-C:H:X. "Volatile" silicon, sulphur and nitrogen depletion, blue photoluminescence, diffuse interstellar bands and ferro-magnetic carbon grain connectionscitations
- 2013On the Excitation and Formation of Circumstellar Fullerenes
- 2013Photoprocessing-driven dust evolution in the diffuse ISM
- 2012Variations on a theme - the evolution of hydrocarbon solids. I. Compositional and spectral modelling - the eRCN and DG modelscitations
- 2012Variations on a theme - the evolution of hydrocarbon solids. II. Optical property modelling - the optEC<SUB>(s)</SUB> modelcitations
- 2012Variations on a theme - the evolution of hydrocarbon solids. III. Size-dependent properties - the optEC<SUB>(s)</SUB>(a) modelcitations
- 2009The Cycle of Carbon Dust in the ISM
- 2008Carbonaceous dust in interstellar shock waves: hydrogenated amorphous carbon (a-C:H) vs. graphitecitations
- 2007IRAS 08572+3915: constraining the aromatic versus aliphatic content of interstellar HACscitations
- 2007Ferromagnetic inclusions in silicate thin films: insights into the magnetic properties of cosmic grainscitations
- 2006The origin of GEMS in IDPs as deduced from microstructural evolution of amorphous silicates with annealingcitations
- 2004Laboratory Studies of the Ion-irradiation of Dust Analogs: Application to the Evolution of Interstellar Silicates
- 2002Temperature-dependent FIR/sub-mm dust emissivity indices: some implications for the diffuse ISM dust compositioncitations
- 2001Structural and chemical alteration of crystalline olivine under low energy He<SUP>+</SUP> irradiationcitations
- 2000The formation and reformation of interstellar dust.
Places of action
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article
Carbonaceous dust in interstellar shock waves: hydrogenated amorphous carbon (a-C:H) vs. graphite
Abstract
Context: Observations of regions of the interstellar medium affected by shock waves indicate gas phase abundances of carbon that are close to solar. In quiescent regions less than half of the carbon is in the gas phase. <BR />Aims: We propose that hydrogenated amorphous carbon (a-C:H), in its many guises, is the most probable form of carbonaceous grain material in the interstellar medium and study its erosion in shock waves. <BR />Methods: We have used the physical properties typical of a-C:H materials, rather than graphite/amorphous carbon, to study a-C:H erosion during ion irradiation and fragmentation in grain-grain collisions. Using SRIM we study material-, surface- and size-dependent sputtering effects and introduce these effects into a shock model. <BR />Results: We find significantly greater destruction for a-C:H, than for graphite, a result that brings the models into better agreement with existing observations of shocked regions of the ISM. Carbon grain erosion in shock waves therefore appears to be much more efficient than predicted by existing models. <BR />Conclusions: Interstellar hydrogenated amorphous carbon dust is, apparently, rather easily destroyed in shocks and must therefore be more rapidly re-cycled and re-formed during its journey through the interstellar medium than previously-thought....