  We calculate the evolution of fluorine in the solar neighborhood with the
\nu-process of core-collapse supernovae, the results of which are in good
agreement with the observations of field stars. The \nu-process operating in
supernovae causes the [F/O] ratio to plateau at [O/H] < -1.2, followed by a
rapid increase toward [O/H] ~ -0.5 from the contribution of Asymptotic Giant
Branch stars. The plateau value of [F/O] depends on the neutrino luminosity
released by core-collapse supernovae and may be constrained by using future
observations of field stars at low metallicities. For globular clusters, the
handful of [F/O] measurements suggest that the relative contribution from
low-mass supernovae is smaller in these systems than in the field.
