Abstract
In the last decade, fullerenes have been detected in a variety of astrophysical environments, with the majority being found in planetary nebulae. Laboratory experiments have provided us with insights into the conditions and pathways that can lead to fullerene formation, but it is not clear precisely what led to the formation of astrophysical fullerenes in planetary nebulae. We review some of the available evidence, and propose a mechanism where fullerene formation in planetary nebulae is the result of a two-step process where carbonaceous dust is first formed under unusual conditions; then, the fullerenes form when this dust is being destroyed.
Highlights
When Kroto et al [1] conducted a series of experiments to simulate the chemistry occurring in the surroundings of carbon-rich evolved stars, they discovered a new and stable carbonaceous molecule: Buckminsterfullerene, C60
Different temperatures result in distinctly different products: no fullerenes are formed at the polycyclic aromatic hydrocarbon (PAH)-favoured temperatures, and no PAHs appear in the high temperature experiments
The circumstellar environments of evolved stars represent what happened to an atomic gas that cooled after ejection due to mass loss processes
Summary
When Kroto et al [1] conducted a series of experiments to simulate the chemistry occurring in the surroundings of carbon-rich evolved stars, they discovered a new and stable carbonaceous molecule: Buckminsterfullerene, C60. Given the stability of the molecule and the nature of the simulation experiments, Kroto et al [1] immediately concluded that C60 was most likely widespread and abundant in space, and as soon as spectroscopic data were available, astronomers searched for its telltale signature in interstellar and circumstellar environments see [2]. Laboratory experiments and astronomical observations have confirmed the identification of two strong (and 3 weaker) diffuse interstellar bands DIBs; see [8] as due to electronic transitions of. Galaxies 2018, 6, 101 know about the conditions that lead to the formation of fullerenes and how this can be reconciled with the body of available observational evidence to construct a coherent formation mechanism for fullerenes in evolved star environments
Sign-in/Register to view highlights & summary Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
