  We demonstrate that by combining two robust theoretical quantum chemistry
calculation techniques, stepwise ionization of C60 fullerene by UV and extreme
UV photons can in principle occur up to a limit as high as q=+26 before coulomb
explosion of the cage. Furthermore, these highly ionized forms exhibit a
comparable structural and bonding stability as for the neutral fullerene.
Certain astrophysical sources like the central stars of planetary nebulae and
the hottest white dwarf stars have sufficiently hard UV radiation fields that
can result in a series of highly charged C60(q+) species from q=1 up to q=16.
Harsher environments, like hot X-ray bubbles in planetary nebulae, X-ray
binaries and other sources, may further push the ionization right up to the
q=+26 limit. These remarkable theoretical findings add new avenues to complex
ion/molecule reactions, the chemistry of fragmentation products and additional
pathways for spreading carbon throughout the universe. The implications for the
emerging field of astrochemistry of C60 fullerene in all its possible states
could be profound.

Astrophysics of Galaxies