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The Stability of Cosmic Fullerenes and Fullerenic Aggregates

Published online by Cambridge University Press:  21 February 2014

E. R. Micelotta ,
J. Cami ,
E. Peeters ,
H. Zettergren ,
H. T. Schmidt ,
H. Cederquist ,
A. P. Jones  and
A. G. G. M. Tielens
E. R. Micelotta
Affiliation:
Department of Physics and Astronomy, University of Western Ontario, London, ON, Canada email: emicelot@uwo.ca
J. Cami
Affiliation:
Department of Physics and Astronomy, University of Western Ontario, London, ON, Canada email: emicelot@uwo.ca
E. Peeters
Affiliation:
Department of Physics and Astronomy, University of Western Ontario, London, ON, Canada email: emicelot@uwo.ca
H. Zettergren
Affiliation:
Department of Physics, Stockholm University, S-106 91 Stockholm, Sweden
H. T. Schmidt
Affiliation:
Department of Physics, Stockholm University, S-106 91 Stockholm, Sweden
H. Cederquist
Affiliation:
Department of Physics, Stockholm University, S-106 91 Stockholm, Sweden
A. P. Jones
Affiliation:
Institut d'Astrophysique Spatiale, CNRS/Université Paris Sud, F-91405, Orsay, France
A. G. G. M. Tielens
Affiliation:
Leiden University, Leiden Observatory, NL-2300 RA Leiden, The Netherlands
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Abstract

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Establishing the stability of cosmic fullerenes and fullerenic aggregates is extremely relevant for a variety of reasons. For instance, the emission features of C60 and C70 fall in the same spectral region as the Un-identified InfraRed (UIR) bands, which they could contribute to. To be able to contribute to the UIR emission, however, fullerenes must be able to survive long enough against the destruction mechanisms operating in the interstellar medium. In this study we focus on the effects of collisional processing, i.e., the bombardment by energetic ions and electrons. A recent experimental/theoretical study has shown that ion collisions with C60 clusters result in the dissociation of the cluster with the simultaneous formation of covalent fullerene dimers, which could play a role as DIBs carriers. We present here our first results about the collisional processing of C60 molecules and clusters by H, He and C ions in interstellar shocks. We have adapted the models that have previously been developed to successfully treat the collisional processing of PAHs in space. The nature of the interaction and the similarities between PAHs and fullerenes make this approach appropriate. In addition, our study shows that the formation of covalent dimers following ion collisions with C60 clusters is compatible with the astrophysical conditions under consideration.

Keywords

ISM: moleculesmolecular processesshock waves
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Symposium S297: The Diffuse Interstellar Bands , May 2013 , pp. 339 - 343
Copyright
Copyright © International Astronomical Union 2014 

References

Cami, J. 2012, Proc. IAU General Assembly Beijing Aug 27–28 , 2012, arXiv:1210.1730Google Scholar
Cami, J., Bernard-Salas, J., Peeters, E., & Malek, S. E. 2010, Science, 329, 1180Google Scholar
Evans, A., van Loon, J. T., Woodward, C. E., et al. 2012, MNRAS, 421, L92Google Scholar
Füller, T. & Banhart, F. 1996, Chem. Phys. Lett., 254, 372Google Scholar
Micelotta, E. R., Cami, J., Peeters, E., et al. 2014, in preparationGoogle Scholar
Micelotta, E. R., Jones, A. P., & Tielens, A. G. G. M. 2010a, A&A, 510, A36Google Scholar
Micelotta, E. R., Jones, A. P., & Tielens, A. G. G. M. 2010b, A&A, 510, A37Google Scholar
Micelotta, E. R., Jones, A. P., & Tielens, A. G. G. M. 2011, A&A, 526, A52Google Scholar
Sigmund, P. 1981, Sputtering by Particle Bombardment Vol.1, ed. Behrisch, R., in Topics in Applied Physics, Vol. 47 (Springer - Verlag)Google Scholar
Zettergren, H., Rousseau, P., Wang, Y., et al. 2013, Phys. Rev. Lett., 110, 185501CrossRefGoogle Scholar