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Fluorine in the solar neighbourhood : Modelling the Galactic thick and thin discs

Grisoni, V. ; Romano, D. ; Spitoni, E. ; Matteucci, F. ; Ryde, N. LU orcid and Jönsson, H. LU orcid (2020) In Monthly Notices of the Royal Astronomical Society 498(1). p.1252-1258
Abstract

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 α-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... (More)

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 α-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 confirmed 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] versus [O/H] plot than in the [F/Fe] versus [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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author
; ; ; ; and
organization
publishing date
type
Contribution to journal
publication status
published
subject
keywords
Galaxy: abundances, Galaxy: evolution
in
Monthly Notices of the Royal Astronomical Society
volume
498
issue
1
pages
7 pages
publisher
Oxford University Press
external identifiers
  • scopus:85096979844
ISSN
0035-8711
DOI
10.1093/mnras/staa2316
language
English
LU publication?
yes
id
e5bc5b19-1f8e-457e-9e3d-bb2d275db38b
date added to LUP
2020-12-11 11:23:59
date last changed
2023-01-01 02:22:00
@article{e5bc5b19-1f8e-457e-9e3d-bb2d275db38b,
  abstract     = {{<p>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 α-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]&lt;−1 has yet to be confirmed 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] versus [O/H] plot than in the [F/Fe] versus [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.</p>}},
  author       = {{Grisoni, V. and Romano, D. and Spitoni, E. and Matteucci, F. and Ryde, N. and Jönsson, H.}},
  issn         = {{0035-8711}},
  keywords     = {{Galaxy: abundances; Galaxy: evolution}},
  language     = {{eng}},
  number       = {{1}},
  pages        = {{1252--1258}},
  publisher    = {{Oxford University Press}},
  series       = {{Monthly Notices of the Royal Astronomical Society}},
  title        = {{Fluorine in the solar neighbourhood : Modelling the Galactic thick and thin discs}},
  url          = {{http://dx.doi.org/10.1093/mnras/staa2316}},
  doi          = {{10.1093/mnras/staa2316}},
  volume       = {{498}},
  year         = {{2020}},
}