Fluorine in the solar neighborhood: modelling the Galactic thick and thin discs. (arXiv:2008.00812v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Grisoni_V/0/1/0/all/0/1">Valeria Grisoni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Romano_D/0/1/0/all/0/1">Donatella Romano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Spitoni_E/0/1/0/all/0/1">Emanuele Spitoni</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Matteucci_F/0/1/0/all/0/1">Francesca Matteucci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ryde_N/0/1/0/all/0/1">Nils Ryde</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jonsson_H/0/1/0/all/0/1">Henrik Jönsson</a>
We investigate the evolution of the abundance of fluorine in the Milky Way
thick and thin discs by means of detailed chemical evolution models compared
with recent observational data. The chemical evolution models adopted here have
already been shown to fit the observed abundance patterns of CNO and
$alpha$-elements as well as the metallicity distribution functions for the
Galactic thick and thin disc stars. We apply them here to the study of the
origin and evolution of fluorine, which is still a matter of debate. First, we
study the importance of the various sites proposed for the production of
fluorine. Then, we apply the reference models to follow the evolution of the
two different Galactic components. We conclude that rotating massive stars are
important producers of F and they can set a plateau in F abundance below
[Fe/H]=-0.5 dex, though its existence for [Fe/H]<-1 has yet to be confimed by
extensive observations of halo stars. In order to reproduce the F abundance
increase in the discs at late times, instead, a contribution from lower mass
stars – single asymptotic giant branch stars and/or novae – is required. The
dichotomy between the thick and thin discs is more evident in the [F/O] vs.
[O/H] plot than in the [F/Fe] vs. [Fe/H] one, and we confirm that the thick
disc has evolved much faster than the thin disc, in agreement with findings
from the abundance patterns of other chemical elements.
We investigate the evolution of the abundance of fluorine in the Milky Way
thick and thin discs by means of detailed chemical evolution models compared
with recent observational data. The chemical evolution models adopted here have
already been shown to fit the observed abundance patterns of CNO and
$alpha$-elements as well as the metallicity distribution functions for the
Galactic thick and thin disc stars. We apply them here to the study of the
origin and evolution of fluorine, which is still a matter of debate. First, we
study the importance of the various sites proposed for the production of
fluorine. Then, we apply the reference models to follow the evolution of the
two different Galactic components. We conclude that rotating massive stars are
important producers of F and they can set a plateau in F abundance below
[Fe/H]=-0.5 dex, though its existence for [Fe/H]<-1 has yet to be confimed by
extensive observations of halo stars. In order to reproduce the F abundance
increase in the discs at late times, instead, a contribution from lower mass
stars – single asymptotic giant branch stars and/or novae – is required. The
dichotomy between the thick and thin discs is more evident in the [F/O] vs.
[O/H] plot than in the [F/Fe] vs. [Fe/H] one, and we confirm that the thick
disc has evolved much faster than the thin disc, in agreement with findings
from the abundance patterns of other chemical elements.
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