Evolution of Fluorine Abundances with the \nu-Process

TL;DR

This study models fluorine evolution in the galaxy, highlighting the role of the u-process in supernovae and AGB stars, and compares predictions with observations in field stars and globular clusters.

Contribution

It introduces a model for fluorine evolution incorporating the u-process, providing insights into fluorine production sources and their dependence on supernova neutrino luminosity.

Findings

/O] ratio plateaus at low metallicity, then rises with AGB star contributions.

The plateau value of [F/O] constrains supernova neutrino luminosity.

Globular clusters show different fluorine contributions compared to field stars.

Abstract

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.