Natural C60 and Large Fullerenes: A Matter of Detection and Astrophysical Implications

Rotundi, A.; Rietmeijer, Frans J. M.; Borg, J.

doi:10.1007/1-4020-4135-7_5

Cited by 6 publications

(4 citation statements)

References 62 publications

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“…According toRotundi et al (2006), fullerenes and carbon nanotubes could be detectable in natural samples using Raman spectroscopy, thanks to a major peak at 1470 cm À1 , and other bands at <1100 cm À1 and >2600 cm À1 . We did not find any evidence for the presence of these bands in L2021C5.…”

mentioning

confidence: 99%

Mid-IR, Far-IR, Raman micro-spectroscopy, and FESEM–EDX study of IDP L2021C5: Clues to its origin

Brunetto

Borg

Dartois

et al. 2011

Icarus

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mentioning

confidence: 99%

Mid-IR, Far-IR, Raman micro-spectroscopy, and FESEM–EDX study of IDP L2021C5: Clues to its origin

Brunetto

Borg

Dartois

et al. 2011

Icarus

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“…The individual fullerene molecules are dispersed in the solid carbon material. C 60 and other fullerenes were frequently identified in particulate carbon samples produced in gas-phase condensation processes such as combustion or in meteorites and interplanetary dust particles (Mordkovich 2000, Rotundi et al 2006, Becker et al 2006. HRTEM image simulations have demonstrated that fullerene molecules produce a ring or doughnut-like structure in the HRTEM (Goel et al 2004, Becker et al 2006, Terrones 2010.…”

Section: Fesem and Hrtem Analysis Of The Residuesmentioning

confidence: 99%

Laboratory Experiments on the Low-temperature Formation of Carbonaceous Grains in the ISM

Fulvio

Góbi

Jäger

et al. 2017

ApJS

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The life-cycle of cosmic dust grains is far from being understood and the origin and evolution of interstellar medium (ISM) grains is still under debate. In the ISM, the cosmic dust destruction rate is faster than the production rate by stellar sources. However, observations of ISM refractory matter suggest that to maintain a steady amount of cosmic grains, some supplementary production mechanism takes place. In this context, we aimed to study possible re-formation mechanisms of cosmic grains taking place at low temperature directly in the ISM. The low temperature condensation of carbonaceous materials has been investigated in experiments mimicking the ISM conditions. Gasphase carbonaceous precursors created by laser ablation of graphite were forced to accrete on cold substrates (T ≈ 10 K) representing surviving dust grains. The growing and evolution of the condensing carbonaceous precursors have been monitored by MIR and UV spectroscopy under a number of experimental scenarios. It is demonstrated, for the first time, the possibility to form ISM carbonaceous grains "in situ". The condensation process is governed by carbon chains that first condense into small carbon clusters and finally into more stable carbonaceous materials, which structural characteristics are comparable to the material formed in gas-phase condensation experiments at very high temperature. We also show that the so-formed fullerene-like carbonaceous material is transformed into a more ordered material under VUV processing. The cold condensation mechanisms here discussed can give fundamental clues to fully understand the balance between the timescale for dust injection, destruction and re-formation in the ISM.

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“…The method allows for the direct imaging of the sample by which one is able to distinguish between amorphous, partly amorphous, and crystalline (mono-or poly-crystalline) phases. TEM observations of carbon soot samples reveal the presence of complex mixed structures such as amorphous grains organized in chain-like aggregates, minor amounts of poorly graphitized carbon and graphitic carbon ribbons, multi-walled onions and fullerenes (Rotundi et al 2006).…”

Section: Electron Microscopymentioning

confidence: 99%

Laboratory studies of simple dust analogs in astrophysical environments

Brucato¹,

Nuth²

2010

Protoplanetary Dust

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Laboratory techniques seek to understand and to place limits upon chemical and physical processes that occur in space. Dust can be modified by long-term exposure to high-energy cosmic rays, thus rendering crystalline material amorphous. It can be heated to high temperatures, thus making amorphous material crystalline. Dust may be coated by organic molecules, changing its spectral properties, or may act as a catalyst in the synthesis of both simple and complex molecules. We describe experimental studies to understand such processes and report studies that focus on the properties of simple oxide grains. We give an overview of the synthesis and characterization techniques most often utilized to study the properties of solids in the laboratory and have concentrated on those techniques that have been most useful for the interpretation of astrophysical data. We also discuss silicate catalysis as an important mechanism that may drive the formation of complex molecular compounds relevant for prebiotic chemistry.

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Natural C60 and Large Fullerenes: A Matter of Detection and Astrophysical Implications

Cited by 6 publications

References 62 publications

Mid-IR, Far-IR, Raman micro-spectroscopy, and FESEM–EDX study of IDP L2021C5: Clues to its origin

Mid-IR, Far-IR, Raman micro-spectroscopy, and FESEM–EDX study of IDP L2021C5: Clues to its origin

Laboratory Experiments on the Low-temperature Formation of Carbonaceous Grains in the ISM

Laboratory studies of simple dust analogs in astrophysical environments

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