Evolution of fluorine in the galaxy with the v-process

We calculate the evolution of fluorine in the solar neighborhood with the v-process of core-collapse supernovae, the results of which are in good agreement with the observations of field stars. The v-process operating in supernovae causes the [F/O] ratio to plateau at [O/H] less than or similar to-1.2,followed by a rapid increase toward [O/H] similar to-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.