Top-down formation of fullerenes in the interstellar medium

Fullerenes have recently been detected in various circumstellar and interstellar environments, raising the question of their formation pathway. It has been proposed that they can form at the low densities found in the interstellar medium by the photo-chemical processing of large polycyclic aromatic hydrocarbons (PAHs). Following our previous work on the evolution of PAHs in the NGC 7023 reflection nebula, we evaluate, using photochemical modelling, the possibility that the PAH C66H20 (i.e. circumovalene) can lead to the formation of the C-60 fullerene upon irradiation by ultraviolet photons. The chemical pathway involves full dehydrogenation of C66H20, folding into a floppy closed cage and shrinking of the cage by loss of C-2 units until it reaches the symmetric C-60 molecule. At 10 from the illuminating star and with realistic molecular parameters, the model predicts that 100% of C66H20 is converted into C-60 in similar to 10(5) yr, a timescale comparable to the age of the nebula. Shrinking appears to be the kinetically limiting step of the whole process. Hence, PAHs larger than C66H20 are unlikely to contribute significantly to the formation of C-60, while PAHs containing between (60) and 66 C atoms should contribute to the formation of C-60 with shorter timescales, and PAHs containing fewer than 60 C atoms will be destroyed. Assuming a classical size distribution for the PAH precursors, our model predicts that absolute abundances of C-60 are up to several 10 4 of the elemental carbon, that is, less than a percent of the typical interstellar PAH abundance, which is consistent with observational studies. According to our model, once formed, C-60 can survive much longer (>10(7) yr for radiation fields below G(0) = 10(4)) than other fullerenes because of the remarkable stability of the C-60 molecule at high internal energies. Hence, a natural consequence is that C-60 is more abundant than other fullerenes in highly irradiated environments.