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Fullerenes in Circumstellar and Interstellar Environments

Published online by Cambridge University Press:  21 December 2011

Jan Cami ,
Jeronimo Bernard-Salas ,
Els Peeters  and
Sarah E. Malek
Jan Cami
Affiliation:
Department of Physics & Astronomy, The University of Western Ontario, London, ON N6A 3K7, Canada email: [email protected] SETI Institute, 189 Bernardo Ave, Mountain View, CA 94043, USA
Jeronimo Bernard-Salas
Affiliation:
Institut d'Astrophysique Spatiale, CNRS/Université Paris-Sud 11, 91405 Orsay, France Cornell University, 222 Space Sciences Bld., Ithaca, NY 14853, USA
Els Peeters
Affiliation:
Department of Physics & Astronomy, The University of Western Ontario, London, ON N6A 3K7, Canada email: [email protected] SETI Institute, 189 Bernardo Ave, Mountain View, CA 94043, USA
Sarah E. Malek
Affiliation:
Department of Physics & Astronomy, The University of Western Ontario, London, ON N6A 3K7, Canada email: [email protected]
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Abstract

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We recently identified several emission bands in the Spitzer-IRS spectrum of the unusual planetary nebula Tc 1 with the infrared active vibrational modes of the neutral fullerene species C60 and C70. Since then, the fullerene bands have been detected in a variety of sources representing circumstellar and interstellar environments. Abundance estimates suggest that C60 represents ~0.1%–1.5% of the available carbon in those sources. The observed relative band intensities in various sources are not fully compatible with single-photon heating and fluorescent cooling, and are better reproduced by a thermal distribution at least in some sources. The observational data suggests that fullerenes form in the circumstellar environments of evolved stars, and survive in the interstellar medium. Precisely how they form is still a matter of debate.

Keywords

astrochemistrycircumstellar matterISM:moleculesinfrared:ISM
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S280: The Molecular Universe , June 2011 , pp. 216 - 227
Copyright
Copyright © International Astronomical Union 2011

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